Class that defines the possible metadata queries specific to the CEDAR data archive.ARO Dat QC4Arecibo data quality code 44592523Channel 3 Calibration (cnt/s over R)Ch3 CalNu20_3000510_1910Vi 5mn aves func(alt) new w coh echoesVn 30-min winds1375_17001ERROR FOR Direction 1 Ion velocity (eastward)error Vi1-1210Vn tides 4-day CEDAR/TIMED analysis1750_17100Te Ti Tn Vi Vn20_15100HtInt HallC2050Height integral hall conductivityNormalized real ACF at lag 12ACFrn12381280_15022Vi Ef Je QjNu Ni Te Ti Faraday rot data > 2000 w coh echoes10_1801Normalized imaginary ACF at lag 123912ACFin121455Vn5hDirection 5 Neutral wind horizontl comp4470_17001Ne Nn Em old optical obs/calcs and transp model inputTn5860_17001842lg(Nmrel)log10 (relative neutral number density)293Y Coord Geocentric Solar MagnetosphericY GSMDirection 7 Neutral wind horizontl compVn7h14756h Tn Phase9976-h max neutral temperature phaselg([O])log10 (O number density)870Na Tn Vn weekly 8-wk Hamming mean days6300_171029658-h max eastward neutral wind phase8h Vne Phs1340_17999Vn tides LTCS period analysisNu72_6313Eastwd Residual Sqrt[1/N*sum(ui-uf)**2]926Vne residNu Ne Ni Te Ti Vi71_7314Wavelength2400WavelengthNu Ne Ni Te Ti Vi73_731480_15616Ne Nn Tn Vi Vn Ef Je Sg cwinds E-reg electro dynMLH Number profile Noise level samples3306NPNSWP831_7001Vi3101JRO W beam log10(1+RxA incoh. pwr/noise)PwrI RxA WNu Ne Ni Te Ti Vi CF73_62063114JRO par 15JRO parameter 153322MLH parameter 23MLH par 23Vn tides 4-day CEDAR/TIMED analysis1221_171003814ACFrn14Normalized real ACF at lag 14ERROR FOR CSL QC Neutral temperature looking Nerror CSL TngN-402372_7116Nu Ne Ni Te Ti ViACFin32Normalized imaginary ACF at lag 3239323588uyneuteSON Error on Uy from signeut3308MLH Number of Radar Sweeps for RecordNRSWP31_3301Nu Ne Te Ti Tr ViNe Tn Sg80_5103MLH parameter 29MLH par 293328MLH Dat QC4Millstone Hill data quality code 4464ERROR FOR 12-h max ion temperature phaseerror 12h Ti Phs-959Ne Nn Te Ti Tn Vi Vn Ef LTCS E reg neu dyn80_15115ACFin9Normalized imaginary ACF at lag 93909Nmlz Alt112Normalizing altitudeEf Ep Sg NH 18-19 Jan 1984311_300103805ACFrn5Normalized real ACF at lag 5Ending azimuth (0=geog N,90=east)133End Azerror el Hem Pwr-365ERROR FOR Estim. Electron Hemispheric Power InputARO Dat QC1Arecibo data quality code 1 (IFIT)456JRO Dat QC4Jicamarca data quality code 4454Ch1 Bright2513Channel 3 line/band brightnessVn tides 4-day CEDAR/TIMED analysis1775_171001140_20001Vn hrly aves, east beam323Ao Index (1 or 2.5 min sample)Aoerror rel Bright-2505ERROR FOR Relative line/band brightness925Number of hours filled in harm analNo hr filld850lg([N2])log10 (N2 number density)Normalized imaginary ACF at lag 8ACFin8390872_6112Nu Ne Ni Te Ti Vi CFlog10 (Vert. integrated electron den.)lg(HtIntNe)52574_7404Nu Ne Ni Te Ti Vihhmm30Hour/min (universal time)ERROR FOR Bisector ion vel (bistatic sys,pos=up)error Vi Bisect-590nangleSON CW angle from GM North for 3626-XY3627Elm pos 1SON Mean elevation position 13519-939error Mean TiERROR FOR Mean ion temperature32_30408Nu Ni Ti Tr ViMinimum altitudeMin Alt10694824h Vnn Amp24-h northward neutral wind amplitudePCI Vostok 60 min polar cap index220_17060UIL QC log10 (Na returns/bkgnd noise)4017lg(Na/bkgd)Tn Em Vn Green line (~96 km, or higher w aurora), EWNS5060_17002SLT@Conj47Local solar time at conjugate point-1282ERROR FOR Direction 8 Ion velocityerror Vi8340APAP index (daily)EcpCharacteristic pos. ion (proton) energy2159Nu Ne Ni Te Ti Tr Vi31_3071Ion temperatureTi552-2561error lg(BkgCnts)ERROR FOR log10 (background counts)-806error Vn SpreadERROR FOR Neutral velocity spreadCyc No95Cycle sequence number (e.g., 5th cycle)Ae320Ae Index (1 or 2.5 min sample)72_6312Nu Ne Ni Te Ti Vi CF-904error lg([Na])ERROR FOR log10 (Na number density)Beg WavenumBeginning wavenumber2411No ACF lags calculatedNo Lags418N Inc IntNo incoherent integrations434710Col FreqIon-neutral collision frequency6320_17100Na Tn climatology aves (1990-1999)error TinfERROR FOR Exospheric temperature-820error Max NeERROR FOR Maximum electron density-530Nu Ne Ni Te Ti Vi71_7118PACE magnetic latitude of meas volumePACE Lat225F10.7 (Sa)F10.7 solar flux (Sa)35073_7210Nu Ne Ni Te Ti Vi1320_17999Vn tides LTCS period analysisSON Error on Ue from signeutueneute3591120_30021sat 1m av IMF (83-88, World Days)4064AQF QC # Quality flag for a night (1-3)AQF QC flag3918ACFin18Normalized imaginary ACF at lag 18Normalized imaginary ACF at lag 27ACFin273927Interpulse PeriodIPP407Smpl Tm usdNo samples used in time average414E Src3501SON EPEC E-Region source code-985ERROR FOR 12-h upward neutral wind amplitudeerror 12h Vnu Amp-934ERROR FOR Mean upward neutral winderror Mean Vnu19Beg mmddBeginning month/day (universal time)lg(ColF)log10 (ion-neutral collision frequency)72031_3303Nu Ne Ni Te Ti Tr Vi2006-10-26T00:00:002006-10-26T00:00:002156Aur Flx TypAuroral flux type: maxwellian=1,gauss=24111PKF QC neut horiz wind fit los to az dirPKF fithlosSON End month/day of composite (UT)End mmdd3539-1475ERROR FOR Direction 7 Neutral wind horizontl comperror Vn7hNe Te Ti Vi40_4203ERROR FOR Direction 4 Ion velocity (perp east)error Vi4-12401230Direction 3 Ion velocity (up)Vi3Te Ti Tn Vi Vn80_15100EIS Dat QC2477EISCAT data quality code 29906h Vne Amp6-h eastward neutral wind amplitudeAdditional increment to rnge gate width126Rng GateIncerror lg(Counts)-2491ERROR FOR log10 (Counts)ERROR FOR Height integral hall conductivity-2050error HtInt HallCMaximum uncorrected electron density531Max Raw Ne180_17002DMSP sat auroral midnight equatorward boundary-1250ERROR FOR Direction 5 Ion velocity (perp north)error Vi59668h Vnn Phs8-h max northward neutral wind phaseERROR FOR Relative background radiance-2555error RelBkgRadnc2155Ee0Average electron energyNn ave 23s, 37.5m6300_7001319Polar Cap IndexPC Index3817ACFrn17Normalized real ACF at lag 17Nu Ne Ni Te Ti Vi73_7208Ne50_510080_15615Nn Tn Vi Vn Ef cwinds 3-pos nuetral dynVn 1988-1993 cubic spline fits5020_17001Vnlos803Line of sight neutral vel (pos = away)RFP los wind before zero rm (+away)RFP losbf04173Vn Red line (~250 km), rel Tn5535_17001820TinfExospheric temperatureFep2133Positive ion (proton) energy fluxDiffuse aurora ratio (Ch1/Ch4)Dif Aur Rat2600Direction 5 Neutral wind horizontl compVn5h1456Uambi3513SON Umerid from ambipolar diffusnERROR FOR 24-h max upward neutral wind phase-987error 24h Vnu PhsARO Dat QC2457Arecibo data quality code 2Tn nightly [O2] aves Maui7191_17094Na Tn monthly means6320_1700374_7710Nu Ne Ni Te Ti ViBeginning year (universal time)Beg Yr9DVS Cloud cover (0-3=clr-ovcst;4=snow)DVS cloud c4132Ne Ni Ti Tr Vi20_2003Solar azimuth angleSol Azimuth181Chatinika/Sondrestrom data qual code 5CHT/SON QC5475Na Tn hourly means6320_17001ERROR FOR Direction 3 Neutral wind (up)-1430error Vn373_7206Nu Ne Ni Te Ti ViNNSAMPMLH Number of noise samples in profile3303ERROR FOR MLH Line of sight Doppler V(pos = away)error Dopp Vel-3350Electron density510Ne3825ACFrn25Normalized real ACF at lag 25Ne Ni Te Ti Vi40_4205No samples used in Fourier transformN Smpl/FFT41710_1101Nu Ne Faraday rot data 19843329MLH par 30MLH parameter 30Nu72_61113832Normalized real ACF at lag 32ACFrn32Nu20_30014SON Total cross correlatn for Ue and Unxccof Uent35819702-dy eastward neutral wind amplitude2dy Vne AmpJRO W beam log10(1+RxB coher. pwr/noise)PwrC RxB W31042070LnInt Ped CField line integral(1 hemi) Ped Cond580VilosLine of sight ion velocity (pos = away)2402Ending wavelengthEnd Wavelen70_6120Vi-1420ERROR FOR Direction 2 Neutral wind (northward)error Vn273_7310Nu Ne Ni Te Ti ViNu Ne Ni Te Ti Vi CF71_6112Vi5F3600SON Direction 5 F Region ion velocityAe (hr)324Ae Index (hourly mean)Nu Ne Ni Te Ti Faraday rot data > 1995 w coh echoes10_1800Nu Ne Te Ti Tr Vi20_30015536log10 (max uncorrected Ne in m-3)lg(RawNmax)Ne Ni Te Ti Tr Tn Vi80_51713913ACFin13Normalized imaginary ACF at lag 13431Code baud lengthCod baud l20_2021Vn LTCS80_15011Vi Eflg(Qparth)log10 (part energy heat rate ht. int.)21412303Pot MaxPotential maximum73TmonnriseUT of Moonrise (from US Naval Obs)50_15051Ef Je Qj Sg71_7206Nu Ne Ni Te Ti ViChannel 4 Calibration (cnt/s over R)2524Ch4 CalAFP QC D(Vne)/Dx per 1000 km (x +Ewrd)DVne/Dx/mkm4056DVS QC Counting error4131DVS cnt errPF NR NoisePKR QC No records in noise avg4002-956error 12h Vne PhsERROR FOR 12-h max northward neutrl wind phaseERROR FOR SON CW angle from GM North for 3626-XY-3627error nangle140Elevation angle (0=horizontal,90=vert)ElNu Ne Ni Te Ti Vi72_7312ACFin29Normalized imaginary ACF at lag 293929V Src3504SON Source of velocityGBF SkyNoisGBF QC Skynoise (A/D convertor units)4031Az(dir 10)Direction 10 Azimuth angle1085Nu Ne Ni Te Ti Vi80_552680_5501Nu Ne Ni Te Ti ViRaw Ne500Uncorrected electron density (Te/Ti=1)Vi newer, mean alt 250 km, 19932930_170022571Channel 1 Background correctionCh1 Bkg CorNu Ne Ni Te Ti Vi CF71_6118Bz GSE2218Interplanetary Mag Field Bz GSE71_7122Nu Ne Ni Te Ti ViNe Ti Tr Vi95_6810120_30012sat hourly IMF and plasma param470STS Dat QC5St. Santin data quality code 5ERROR FOR Electron densityerror Ne-510923GrovsCoefNoGroves coefficient number310_10034Ne Ni Nn Te Ti Tn Vn Ep 22 March 1979Vn tides LTCS period analysis1620_179991240_17001VnAFP I Cal FAFP QC Intensity Calibration Factor4053Normalized real ACF at lag 3ACFrn33803error Ln int J5-1950ERROR FOR Line int (1 hemi): dir 5 current den10_1040Vi175_31012DMSP sat electron hemispheric power in GW903lg([N(2D)])log10 (N(2D) number density)1280Vi8Direction 8 Ion velocityVi Ef Je Qj Qp Sg50_15021Ni Nn Te Ti Tn Vi Vn31_15100ERROR FOR Ion Composition - [O+]/Neerror [O+]/Ne-620Nu Ne Ni Te Ti Vi CF73_6306PACE Lon245PACE magnetic longitude of meas volume74_6404Nu Ne Ni Te Ti Vi CF244Geom LonGeomagnetic (cntrd dipol) east longitudIon Composition - [mol wt 28 to 32]/Ne[N-0]/Ne690DDSOPeNDAP DDS (Data Descriptor Structure) data fileNu Ne Ni Te Ti Vi CF73_6210S/N411Signal to noise ratioDirection 1 Ion velocity (eastward)Vi11210Emery intersat adjust hourly composite elec Hp175_31200Al321Al Index (1 or 2.5 min sample)Vi Ef Viperp(>180km, 0.25 mlat bins), Vipar=080_1563012h Tn Phs12-h max neutral temperature phase95741_30004TnPeak PowerPeak power486480EIS Dat QC5EISCAT data quality code 572_6305NuRange Inc121Additional increment to rangeNu Ne Ni Te Ti Vi72_72083926ACFin26Normalized imaginary ACF at lag 26Nu Ne Ni Te Ti Vi CF74_6710Tn Em Vn (some Vn only line-of-sight)5480_7001Scale ht of Chapman model electron den541Ht Scl Chap-44ERROR FOR Local solar timeerror SLT445Aurora SeenAurora sighted Flag (0=no, 1=yes)-720error lg(ColF)ERROR FOR log10 (ion-neutral collision frequency)Direction 4 Ion velocity (perp east)1240Vi42-day component period2dy Period980NICT %th crNICT QC % threshold acceptance criteria415220_30008Ne Ni Te Ti80_5121Ne Ni Te Ti Tr Tn Vi71_6120Nu Ne Ni Te Ti Vi CF24561/2-wid DevRelative 1/2-width deviation from 245595512h Vne Phs12-h max eastward neutral wind phase310_11062Tn Vn Ep tides 60kV-1450ERROR FOR Direction 5 Neutral wind (perp north)error Vn5Ne Ni Te Ti Vi pre-LTCS50_150143802Normalized real ACF at lag 2ACFrn2INFOOPeNDAP information data fileSW Vy GSMSolar Wind velocity GSM y component2246lg(F Factr)UIL QC log10 (F factor)4016Integration time for these dataInt Time6071_6206Nu Ne Ni Te Ti Vi CF3514Uden1SON Uambi from DNe/DH fit to neNu Ne Ni Te Ti Vi CF73_6314ERROR FOR Direction 6 Neutral winderror Vn6-1460error VnlosERROR FOR Line of sight neutral vel (pos = away)-800Vn Tn vector hourly means6320_18011Nu72_6119Ne Sg80_5102CSL QC Full Width at Half Max vert avgCSL FWHMzav4021425Wide Chi SqWide reduced-chi square of fitNu Ne Te Ti Tr Vi31_3001EIS Dat QC1476EISCAT data quality code 1130Mean azimuth angle (0=geog N,90=east)Az1272Direction 7 Ion velocityVi7ERROR FOR log10 (Ne in m-3)-520error lg(Ne)530Max NeMaximum electron densityDirection 5 Neutral wind (perp north)1450Vn5Maximum altitude108Max AltVn2Direction 2 Neutral wind (northward)1422Ped Cond2010Pedersen conductivityerror Vilos Inc-581ERROR FOR Additional increment to code 58073_7306Nu Ne Ni Te Ti ViNe Ti Tr Vi95_6801Groves coefficient924Grovs Coef-4004error lg(NoisPwr)ERROR FOR PKR QC log10 (noise pwr in spectrm)Solar Wind Plasma SpeedSol Wnd Spd223424h Vne Amp94324-h eastward neutral wind amplitude72_6311Nu72_7314Nu Ne Ni Te Ti Vi4025CFP QC No coefficientsCFP N CoefsSON Correlation coefficient Exyc cof Exy35752511Ch1 BrightChannel 1 line/band brightness3593siguetotSON Total error on UeNa Tn Vn6300_171013517UgravSON portion of Uambi from gravityDirection 6 Neutral wind1460Vn672_7306Nu Ne Ni Te Ti Vi95_30001Ne Ti Tr ViTsset NautUT of Nautical sunset (szen=102 deg)76-650error [HE+]/NeERROR FOR Ion Composition - [HE+]/Ne511Additional increment to code 510 (Ne)Ne IncHem PwrQualEstimated Hemispheric Power Qualifier367Ef Ep Qp Sg SH 20-21 Mar 1990311_30022-1422ERROR FOR Direction 2 Neutral wind (northward)error Vn2IMF 1min S/C SW: Den!Vx IDx IDyz4122IMF1 S/C SW72_7118Nu Ne Ni Te Ti ViNormalized imaginary ACF at lag 23902ACFin2Vi820_700112h Vnu Amp12-h upward neutral wind amplitude985-989ERROR FOR 12-h max upward neutral wind phaseerror 12h Vnu Phs-1412error Vn1ERROR FOR Direction 1 Neutral wind (eastward)24-h eastward neutral wind amplitude94024h Vne Amp1030Az(dir 7)Direction 7 Azimuth angle3807Normalized real ACF at lag 7ACFrn7Vi910_70016330_17001Nn Tn nightly means981UT day no rel to 2-dy comp phased# 2d Phase80_9003Nu1140_20003Vn hrly aves, vertical beam-955error 12h Vne PhsERROR FOR 12-h max eastward neutral wind phaseCloud CoverCloud cover (0-8=clr-ovcst;9=obscured)440-976ERROR FOR 2-dy max northward neutrl wind phaseerror 2dy Vnn Phs2930_17001Vi older, mean alt 300 km, 1989Vi870_7001error RFP losbf0-4173ERROR FOR RFP los wind before zero rm (+away)1210_17999Vn tides LTCS period analysisEstim. Total Hemispheric Power Inputtot Hem Pwr3633821Normalized real ACF at lag 21ACFrn21lg([Na])904log10 (Na number density)66DT rowsTime increment between rowsWidth of range gate125Rng GateACFrn11Normalized real ACF at lag 113811Tn5980_17001Nu Ne Ni Te Ti Vi73_7118ERROR FOR STM QC Solar scaling factorerror STM sol scl-408073_7120Nu Ne Ni Te Ti ViPower NrmKMLH D.P. Power Normalization constant33182090_17001Vn tides normal analysisNu Ne Ni Te Ti Vi73_7112lg(Mn)log10 (neutral mass density)830-500ERROR FOR Uncorrected electron density (Te/Ti=1)error Raw Ne430Goodnes FitGoodness of fit12h Vne Amp95012-h eastward neutral wind amplitude71_6310Nu Ne Ni Te Ti Vi CFMLH ACF Normalization Factor3313ACF NormERROR FOR Direction 2 Neutral wind (northward)-1421error Vn2Direction 7 Elevation angle1040El(dir 7)Alt AvgNtvl115Altitude averaging intervalNu Ne Ni Te Ti Vi CF73_6118871scale factor to model [O] profile[O] mod sclEm Vn5160_17020SW Vx GSMSolar Wind velocity GSM x component2244Vn tides monthly climatology (78-82)1620_1700180Time delayTdelay80_15414Ne Te Ti Vi LTCS E reg alter code6300_17003Fe ave 15mn, 525mnone170_8017St. Santin data quality code 3468STS Dat QC33801Normalized real ACF at lag 1ACFrn1Local solar timeSLT44Tn Vn Ep 60kV310_110614165EHP origHPeEHP original estim. Electron Hp inputRelative line/band brightnessrel Bright2505A contour plot of the selected variable versus Height (Y axis) and Time (X axis)Height vs TimeA contour plot of the selected variable versus Height (Y axis) and Time (X axis)70_6312Vi412lg(S/N)log10 (signal to noise ratio)900_7001ViTemperature ratio (Te/Ti)570Te/Ti42_30004TnNu Ni Ti Tr Vi MIDAS-W anal31_341072_7122Nu Ne Ni Te Ti Vi406Spct Smpl TSpectral sampling time5950_17001Tn6-h max eastward neutral wind phase6h Vne Phs99572_6306Nu Ne Ni Te Ti Vi CFSON Derivative of Te with altitudeDTe/DHt3511Northwd Residual Sqrt[1/N*sum(vi-vf)**2]Vnn resid927CHT/SON QC2472Chatanika/Sondrestrom data qual code 2Tn5900_17001-1440ERROR FOR Direction 4 Neutral wind (perp east)error Vn4Poker Flat AK I.S. Radarhttp://cedarweb.hao.ucar.edu3907Normalized imaginary ACF at lag 7ACFin75340_7001Tn Em Vn vertical meas in zero vel ref-2507ERROR FOR Relative line emission rateerror LinEmisRaterror F10.7 (Sa)-350ERROR FOR F10.7 solar flux (Sa)c cof xySON Correlation coefficient vxy3571AQF QC # Samples in time avg of 14111411 # vals4061224Geom LatGeomagnetic (centered dipole) latitude70_6210ViMLH parameter 8MLH par 83307No. samples in dir. 1 avg. (eastward)NoSmpl Dir14224035GBF GScat FGBF QC Groundscatter flag (0:n, 1:y)Ne Te Ti Vi Ef cwinds 3-pos long pulse80_15613Nu Ne Ni Te Ti Vi CF72_6122Nu Ne Ni Te Ti Vi72_8000Beginning azimuth (0=geog N,90=east)132Beg Azxccof UenSON Cross correlation coefficient Une3577Nu Ne Ni Te Ti Vi CF71_6210Neutral velocity spreadVn Spread805Sampling interval (time between sampls)Sampl Ntvl7024-h ion temperature amplitude94424h Ti Amp32_30420Nu Ni Ti Tr ViCh4 WavelenChannel 4 Wavelength2424Ne Te Ti Vi40_4202VnlosLine of sight neutral vel (pos = away)80080_5503Nu Ne Ni Te Ti Vi4473_18002Ne Nn Strickland transport model inputs w 2 locschi sq Ne3566SON Reduced chi square of NeACFrn15Normalized real ACF at lag 153815Nu Ne Ni Te Ti Vi CF72_640270_6122ViAz Change135Variation in azimuth (end Az - beg Az)GBF QC XCF flag (0=Off, 1=On)4032GBF XCF FlgACFin103910Normalized imaginary ACF at lag 103831Normalized real ACF at lag 31ACFrn3195_6800Ne Ti Tr Vi6300_17001Nn ave 15mn, 525mSmpl Tm UsdNo smpls in time avg; or 414 incremnt415402Pulse length2006-10-26T00:00:002006-10-26T00:00:00Pulse Len2401Beg WavelenBeginning wavelength1230_17999Vn tides LTCS period analysis71_7120Nu Ne Ni Te Ti Vi175_31021NOAA sat tot, elec and proton hem power in GWNe Ni Te Ti Vi LTCS80_15014Nu Ne Ni Te Ti Vi CF72_631498424h Vnu Amp24-h upward neutral wind amplitude5160_17001Em Vn older submissionsNe Ti Tr Vi95_30031ERROR FOR 2-dy eastward neutral wind amplitude-970error 2dy Vne AmpSON Uambi from DNe/DH fit to ln(ne)Uden23515Tn nightly [OH] aves Maui7191_17087lg(NaCount)4015UIL QC log10 (sodium counts)3321MLH par 22MLH parameter 22Nu80_90051080El(dir 9)Direction 9 Elevation angleF10.7 Multiday average observedF10.7a356Arecibo data quality code 5ARO Dat QC5460End hhmmSON End hour/minute of composite (UT)3540Tn Vn LTCS Azeem/Johnson analysis80_30024441CloudCover1Cloud cover from lowest level clouds292X Coord Geocentric Solar MagnetosphericX GSMPKR QC log10 (signl pwr in spectrm)lg(SgnlPwr)4005-2456ERROR FOR Relative 1/2-width deviation from 2455error 1/2-wid DevRaw NeUncorrected electron density502MlatEqBndryEst mag lat 0MLT equatorwd aurora bndry370lg([N(4S)])log10 (N(4S) number density)902-3513error UambiERROR FOR SON Umerid from ambipolar diffusnNu Ne Ni Te Ti Vi CF74_7000JRO E beam log10(1+RxD coher. pwr/noise)PwrC RxD E310871_6116Nu Ne Ni Te Ti Vi CFTsset AstrUT of Astronomical sunset (szen=108 deg)786-h neutral temperature amplitude6h Tn Amp992Fe ave 23s, 37.5m6300_700337Beg TimeIncAdditional increment to time past 0 UT71_6122Nu Ne Ni Te Ti Vi CFNu Ne Ni Te Ti Vi74_76043518Azm pos 1SON Mean azimuth position 1110AltitudeAltitude (height)4470_17002Ne Nn Em optical obs/calcs and transp model inputMLH Mean power prof Normalizatn Const3310PNRMMPNn Tn hourly means6330_17002107Min Alt IncAdditional increment to min altVn hrly aves, north beam1140_20002Time past 0000 UTTime > 0UT34Day number of year (universal time)Day No211420Vn2Direction 2 Neutral wind (northward)Peach MountainPeach Mountain is the home of the 24 inches McMath Telescope and is part of Stinchfield Woods. Stinchfield Woods is owned by the University of Michigan and used by several university departments including the Astronomy Department and the School of Natural Resources and Environment.http://www.umich.edu/~lowbrows/theclub/mcmath.htmlerror lg(rel br)ERROR FOR log10 (Relative line/band brightness)-2506327Ao Index (hourly mean)Ao (hr)Direction 8 Elevation angleEl(dir 8)10606-h max northward neutral wind phase6h Vnn Phs996UT at start of 2-day comp calcBegUT 2dcal982ERROR FOR Direction 1 Neutral wind (eastward)-1410error Vn1AFP QC Error in 4056/4057 per 1000 km40584056-7ErrorNa Tn Vn monthly 8-wk Hamming mean days6300_17103-940error 24h Vne AmpERROR FOR 24-h eastward neutral wind amplitude4473_17002Ne Nn Em optical obs/calcs and transp model inputERROR FOR log10 (uncorrected electron density)error lg(RawNe)-505ERROR FOR AP index (daily)error AP-340Nu Ni Ti Tr Vi MIDAS-W anal32_341072_6115Nu3820Normalized real ACF at lag 20ACFrn20Mean ion temperatureMean Ti93924h Tn Phs94724-h max neutral temperature phase20_2011Vi6320_17011Na Tn Vn los hourly meansChannel 2 line/band brightness2512Ch1 BrightERROR FOR Direction 3 Corrupt Neutral wind (up)-1432error Vn3c1050Az(dir 8)Direction 8 Azimuth angleMLH par 6MLH parameter 63305Nu80_900212h Vnn Amp95112-h northward neutrl wind amplitudeJRO parameter 163115JRO par 16SON Direction 4 F Region ion velocityVi4F3599aa341aa indexACFin15Normalized imaginary ACF at lag 153915NICT QC 1-h std dev rejection criteriaNICT std cr41513516UtempSON portion of Uambi from dTp/dHNe Ti Tr Vi95_68313583UzneuteSON Alternate error on Uzum (code 1460)5465_17001Tn Em Vn80_5150Ne31_13002Vi EfERROR FOR Direction 7 Ion velocity-1270error Vi7Ch1 WavelenChannel 1 Wavelength2421Ch2 Bkg CorChannel 2 Background correction2572113Nmlz AltIncAdditional increment to normalizing altKp, ap, Ap, F10.7 solar flux (daily,3 cycles)210_30007BdecGeomagnetic field east declination213ion Hem Pwr364Estim. Ion Hemispheric Power Input1070Az(dir 9)Direction 9 Azimuth angleAzm pos 23520SON Mean azimuth position 273_6402Nu Ne Ni Te Ti Vi CF1340_17100Vn tides 4-day CEDAR/TIMED analysis550Ion temperatureTiVn1Direction 1 Neutral wind (eastward)14103536Beg hhmmSON Begin hour/minute of composite (UT)71_7116Nu Ne Ni Te Ti Vinone170_8016DTi/DHt3510SON Derivative of Ti with altitude1252Vi5Direction 5 Ion velocity (perp north)80_5523Nu Ne Ni Te Ti Vi acport ac elscansTn Em Vn5300_700280_15116Ne Nn Tn Vi Vn Ef Je Sg LTCS E reg electrodyn10_1802Nu Ni Te Ti1320_17012Vn hourly winds > 5/98Flat space-delimited data fileFLAT80_15614Ne Te Ti Vi cwinds 3-pos ac multi pulse142Beginning elevation angleBeg ElEISCAT data quality code 4EIS Dat QC447971_6402Nu Ne Ni Te Ti Vi CF24h Vnu Amp24-h upward neutral wind amplitude986423NoSmpl Dir2No. samples in dir. 2 avg. (northward)72_6205NuNu Ne Ni Te Ti Vi72_7206Vn tides d/sd func(altitude) > 5/981320_17013Emery intersat adjust elec,SEM-2 ion Hp (GW)175_311003574Neut AtmSON Neutral atmosphere model code4112PKF fitpvnlPKF QC perp (left) compon. to code 411110_1051ViACFin30Normalized imaginary ACF at lag 3039301539_17100Vn tides 4-day CEDAR/TIMED analysis458ARO Dat QC3Arecibo data quality code 32506log10 (Relative line/band brightness)lg(rel br)Vi845_7001error Tn1-812ERROR FOR Neutral temperature71_7210Nu Ne Ni Te Ti Vi3116JRO par 17JRO parameter 17ACFin23Normalized imaginary ACF at lag 233923806Neutral velocity spreadVn SpreadERROR FOR Joule energy heat rate height integralerror Qjoulh-2150432No. bauds in codeCod baud n321_20001Tn Vn tides2090_17999Vn tides LTCS period analysis499Nm lshot/sNumber of laser shots per secondChannel 3 Wavelength2423Ch3 WavelenSolar Wind velocity GSM z componentSW Vz GSM2248xccof Uxyn3578SON Cross correlatn on Uxy from signeutF10.7q(Sa)F10.7 solar flux qualifier3511260Direction 6 Ion velocity (antiparallel)Vi6error 24h Ti Phs-949ERROR FOR 24-h max ion temperature phaseMagnetic unit vector rotation angleRot angl-mg102050_5103Ne Tn SgVel Az600Velocity direction - local azimuth811Tn ModelModel Neutral temperature3928ACFin28Normalized imaginary ACF at lag 281390_17100Vn tides 4-day CEDAR/TIMED analysiserror Vi4FERROR FOR SON Direction 4 F Region ion velocity-35991/2 Scat A190Half scattering angle (bistatic system)SON Error on Un from signeut3592unneute5000_17111Tn Em Vn Red line (~240 km), multi-directionsEnding elevation angle143End El-690ERROR FOR Ion Composition - [mol wt 28 to 32]/Neerror [N-0]/Ne2491log10 (Counts)lg(Counts)Invariant latitude in measurement vol222Inv LatMUI QC (0-3 <=> ok-bad)MUI qc4092Cloud cover in tenths (0=clr,10=ovcst)cloudcov10442Tn Vn tides322_200012232Sol Wnd DenSolar Wind Plasma DensityEIS Dat QC3478EISCAT data quality code 372_6209NuInterplanetary Mag Field By GSEBy GSE2216365el Hem PwrEstim. Electron Hemispheric Power Input-1610error E1ERROR FOR Direction 1 electric field (eastward)Number of directions in analysis922No Dirs-941ERROR FOR 24-h northwrd neutral wind amplitudeerror 24h Vnn Amp498Number of frequencies usedNum FreqNormalized imaginary ACF at lag 4ACFin43904Nu Ne Ni Te Ti Vi CF72_61167191_17001Tn nightly [OH] aves Ft CollinsNa ave 15mn, 525m6300_1700295_30010Ne Ti Tr ViNu Ne Ni Te Ti Vi80_550573_7122Nu Ne Ni Te Ti ViTab delimited data fileTABCSL QC Neutral temperature looking NCSL TngN4023Ending wavenumber2412End Wavenumlog10 (background counts)2561lg(BkgCnts)ACFrn30Normalized real ACF at lag 303830127Rng Gate NoRange gate numberGeodetic latitude of measurementGeod Lat160311_30019Ep SH assumed 23-26 Sep 198650_5124Te TiVn tides 4-day CEDAR/TIMED analysis1245_17100J5Direction 5 electric current density1850error TiERROR FOR Ion temperature-552Alt Avg Inc116Additional increment to ht avgng intrvlParticle energy heat rate hemisph.int.Qparthe2142MUSCOX Fit Code473Fit Code3350Dopp VelMLH Line of sight Doppler V(pos = away)ERROR FOR MLH parameter 52-3351error MLH par 52ERROR FOR Direction 4 Ion velocity (perp east)error Vi4-1241MLH par 21MLH parameter 2133201411 s dev4060AQF QC Standard deviation in 1411Em Vn combined meas in zero vel ref5160_17010Normalized imaginary ACF at lag 5ACFin53905Te Ti80_5174Nu72_630912h Gp Phs95812-h max geopotential phasePotential minimumPot Min230294924-h max ion temperature phase24h Ti PhsRFP avlosh4172RFP ave hourly zero los winderror Vn SpreadERROR FOR Neutral velocity spread-805MLH parameter 54MLH par 543353Wide ChiSqi426Additional increment to wide chi square3346MLH lagMLH Lag spacingSTM sol scl4080STM QC Solar scaling factorerror lg(Bright)ERROR FOR log10 (line/band brightness)-2501MLH parameter 263325MLH par 26AFP QC No Harmonics in Fourier Anal4055AFP No HarmSON Correlation coefficient vyzc cof yz3573COF ts wnd4070COF QC Mean sampling density for windsNu Ne Ni Te Ti Vi73_7502-935error Mean VneERROR FOR Mean eastward neutral wind12-h max upward neutral wind phase12h Vnu Phs9891220Vi2Direction 2 Ion velocity (northward)Nu Ne Ni Te Ti Vi72_712072_7402Nu Ne Ni Te Ti Vi[H+]/NeIon Composition - [H+]/Ne66025_17000ViCSL Tnav4020CSL QC Neutral temperature from 1-hr avgerror E2-1620ERROR FOR Direction 2 electric field (northward)360Sunspot numberSunspot noJoule heat rate hemisphere integratedQjouhe215270_6314Vilog10 (AR number density)880lg([AR])30_13021Vn tides LTCS80_9001NuSON log10 (ne-parabolic fit to ln(ne))3568lg(fit(Ne))Neutral gas mean molecular weight829GMWn2455Refernce rel 1/2-width (arb press unit)Ref 1/2-wid72_6118Nu Ne Ni Te Ti Vi CFPlot of parameter values vs time coordinateTime Series54Mag LocalMagnetic local time467STS Dat QC2St. Santin data quality code 2error Vnlos-802ERROR FOR Line of sight neutral vel (pos = away)error Vi2ERROR FOR Direction 2 Ion velocity (northward)-1220Nu Ne Te Ti Tr Vi32_300195212h Tn Amp12-h neutral temperature amplitude10_1911Vi 4 ht avs kindat 1910 w/o coh echoesNu Ne Ni Te Ti Vi73_7116Tn Em Vn5300_7003Vn tides 4-day CEDAR/TIMED analysis1310_17100Nu Ne Ni Te Ti Vi CF74_6604IMF/SW QualIMF/Solar Wind Qualifier2236Millstone Hill data quality code 3463MLH Dat QC3Tn Vn Red line (~240 km), vertical5510_17001Nu Ne Ni Te Ti Vi CF73_6310H4P SZ flgHecht 4ch Ph. 1=ok (sza>102;flux;Eo;fo)4102error TiERROR FOR Ion temperature-550SON Source of temperature3503T SrcNormalized real ACF at lag 43804ACFrn41250Vi5Direction 5 Ion velocity (perp north)Geodetic longitude of measurementGeod Lon170G Circ DstHoriz great crcl dist from ref lat/lon150Nu Te Ti Vi53_9801Ne Te Ti Vi Ef LTCS F reg long pulse80_1541312h Vne Phs12-h max northward neutrl wind phase956Vi911_7001sat 1m av IMF and plasma param120_30027Vn tides 4-day CEDAR/TIMED analysis1375_17100Tn Vn Ep tides 90kV310_11092Tn Em Vn Red line (~240 km), cardinal dirs5060_17001Ni Te Ti Vi Ef20_30001MLH Mode Letter (65-80 = A-P)MLH Mode3300ERROR FOR SON E Field Magnitude (XY plane)error XY |EF|-3628ERROR FOR Electron density-512error NeMean northward neutral wind936Mean Vnn825_7001ViChi SqrReduced-chi square of fit420220_17001PCI Vostok 1 min polar cap index32_15100Ni Nn Te Ti Tn Vi VnVi10Direction 10 Ion velocity13002-dy max eastward neutral wind phase9752dy Vne Phs3572SON Correlation coefficient vxzc cof xz12-h max ion temperature phase12h Ti Phs959AFP QC Zenith ref flag (1=use ; 0=no)4050AFP Zen FlgVertically integrated electron density524Vert Int Ne1431Vn3Direction 3 Neutral wind (up)Vn Tn vector nightly means6320_1801271_6314Nu Ne Ni Te Ti Vi CF30_13210Vi Vn EfNormalized imaginary ACF at lag 24ACFin243924log10 (integrated electron density)523lg(Int Ne)Normalized Brightness ratio (Ch1/Ch4)NorBritnRat2601ERROR FOR Direction 4 electric field (perp east)error E4-1640By GSMInterplanetary Mag Field By GSM2206Nu Ne Ni Te Ti Vi CF71_631271_7310Nu Ne Ni Te Ti ViVn tides mean and sd f(v alt) > 5/981320_170115480_7002Tn Em VnE51650Direction 5 electric field (perp north)Beg TimeInc31Centiseconds (UT, increment to hhmm)Beg csecSON Begin centisecond of composite (UT)3537F10.7 ObsF10.7 solar flux observed (Ottawa)354330DstDst indexerror 24h Vnu AmpERROR FOR 24-h upward neutral wind amplitude-9843324MLH par 25MLH parameter 25-1230error Vi3ERROR FOR Direction 3 Ion velocity (up)80_15013Ne Ni Te Ti Vi Ef LTCS F regionNu Ne Ni Te Ti Tr Vi32_3303Nu Ne Ni Te Ti Vi80_5506Vn tides 4-day CEDAR/TIMED analysis1285_17100Sol ZenithSolar zenith angle in measurement vol18030_13212Vi Vn Ef LTCS F regionACFin223922Normalized imaginary ACF at lag 2272_6501Nuerror VilosERROR FOR Line of sight ion velocity (pos = away)-580BdDownward component of geomagnetic field208-975ERROR FOR 2-dy max eastward neutral wind phaseerror 2dy Vne PhsNe50_5101Nu Ne Ni Te Ti Vi80_55023829ACFrn29Normalized real ACF at lag 29465Millstone Hill data quality code 5MLH Dat QC53594siguntotSON Total error on UnModl Day NoModel Day number of year (UT, 1=Jan 1)223903ACFin3Normalized imaginary ACF at lag 3ERROR FOR log10 (O2 number density)error lg([O2])-86070_6208Vi5015_17011Tn Vn Red line (~240 km), multi-directions311_30018Ef Ep Qp Sg new NH 23-26 Sep 1986Estimated Hemispheric Pwr Corr. Factor368Hem PwrFctrMLH Dat QC2462Millstone Hill data quality code 2ERROR FOR line/band brightness-2502error Bright84Daily mean time delayTdelay dayChi Sqr421Reduced-chi square of fit74_6709NuERROR FOR Ion Velocity spread (spectral width)-585error Vi Spread-842ERROR FOR log10 (relative neutral number density)error lg(Nmrel)Joule energy heat rate height integralQjoulh2150204BnNorthward component of geomagnetic fldlg([O2])860log10 (O2 number density)xccof UxytSON Total cross correlation for Uxy3579ACFrn23Normalized real ACF at lag 233823MUI Vi3-ewMUI QC Ion velocity (up from EW dirs)4091Direction 4 electric field (perp east)E416402140QparthParticle energy heat rate height int.Vi70_6118Nu Ni Ti Tr Vi32_3408UT of Civil sunset (szen=96 deg)74Tsset CivilCOF QC Mean sampling density for htsCOF ts hts4071Tn nightly averages3320_17004-870error lg([O])ERROR FOR log10 (O number density)1275_17001Vn 30-min windserror lg([N2])-850ERROR FOR log10 (N2 number density)error lg(SgnlPwr)ERROR FOR PKR QC log10 (signl pwr in spectrm)-4005Vn1215_17001Normalized imaginary ACF at lag 31ACFin3139312890_17002Vi1432Direction 3 Corrupt Neutral wind (up)Vn3cNu Ne Ni Te Ti Vi CF71_6502error relativ Tn-813ERROR FOR Relative neutral temperatureVn1254_17001[O2+]/NeIon Composition - [O2+]/Ne64080_5521Nu Ne Ni Te Ti Vi3919Normalized imaginary ACF at lag 19ACFin19Ne Ni Ti Tr Vi20_2002-936ERROR FOR Mean northward neutral winderror Mean Vnnaxis of symSON Azimuth of axis of symmetry35975540_7001Tn Vn953log10 (12-h geopotential amplitude)lg(12h Gp)lg(Ne)log10 (Ne in m-3)5203828ACFrn28Normalized real ACF at lag 2831_3302Nu Ne Ni Te Ti Tr Vi6300_7002Na ave 23s, 37.5mPwrI RxD EJRO E beam log10(1+RxD incoh. pwr/noise)31074163EHP original estim. Total Hp inputEHP origHpt3818ACFrn18Normalized real ACF at lag 18Stream binary fileSTREAMERROR FOR MLH ACF Normalization Factor-3313error ACF Norm1040_2002VnNe Ni Te Ti Vi Ef50_15013Receiver bandwidth494Rec BandwCh4 Bkg CorChannel 4 Background correction2574Normalized real ACF at lag 63806ACFrn6PwrI RxB WJRO W beam log10(1+RxB incoh. pwr/noise)3103Scan TypeScan type (0=any,1=fixed,2=az,3=el)9480_19120Vi Ef Je Sg3113JRO parameter 14JRO par 14PF Gal NoisPKR QC Avg of Galactic Noise40034124IMF 1min S/C delay: d!Bx IDdel IDmeandelIMF1 S/Cdel3302MLH Number of signal samples in profileNRP3351MLH parameter 52MLH par 52MLH Additional increment to DP Pwr Nrm C3319Additnl P.error Alt Inc-111ERROR FOR Additional increment to altitudeZ GSEZ Coordinate Geocentric Solar Ecliptic29730_15100Ni Nn Te Ti Tn Vi Vn3809ACFrn9Normalized real ACF at lag 9461MLH Dat QC1Millstone Hill data quality code 1311_30020Vi Ep Qp SH,NH 23-26 Sep 1986 for TIGCMVn tides mean winds, normal anal1220_17001-1650error E5ERROR FOR Direction 5 electric field (perp north)error uycorr-3586ERROR FOR SON Correction term = Uy-VyuxneuteSON Error on Ux from signeut3587MUI QC Ion velocity (up from NS dirs)4090MUI Vi3-ns95_30131Ne Ti Tr ViSON Relative error in neutral atmossigneut3595ACFin1Normalized imaginary ACF at lag 13901Electric Potential2310Elect Pot3906Normalized imaginary ACF at lag 6ACFin6Mean neutral temperature937Mean Tn43_30004Tn1390_17999Vn tides LTCS period analysis20_2010Ne Ni Te Ti ViSON FIT CodeFIT Code35002dy Vnn Phs2-dy max northward neutrl wind phase9763921Normalized imaginary ACF at lag 21ACFin21SON Ion gyro frequency3596ion g freq-3629ERROR FOR SON CW angle from GM North for 3628-XYerror EF nangleLnInt HallCField line integral(1 hemi) Hall Cond2080ERROR FOR Electron temperatureerror Te-560490Xmit FreqTransmitted frequency2422Ch2 WavelenChannel 2 Wavelength1215_17100Vn tides 4-day CEDAR/TIMED analysis410Signal to noise ratioS/N3582UmeridSON Horizontal magn neutral windPosition number within cyclePos No961421 # valsAQF QC # Samples in time avg of 14214063120RangeRange220_17015PCI Vostok 15 min polar cap index73_7402Nu Ne Ni Te Ti ViVn tides1560_17001UT of Astronomical sunrise (szen=108deg)79Tsris AstrNeutral temperatureTn810Vn tides 4-day CEDAR/TIMED analysis1240_171003538SON End year of composite (UT)End yr compHecht 4ch Ph. Model no. (eg MSIS90)4101H4P mod noerror 24h Vnn PhsERROR FOR 24-h max northwrd neutral wind phase-946Nu Ne Ni Te Ti Vi CF71_6208Nu Ne Ni Te Ti Vi71_7502error AltitudeERROR FOR Altitude (height)-11031_13001Vi EfAdditional increment to code 580581Vilos Inc452Jicamarca data quality code 2JRO Dat QC25510_10012Tn Vn Unchecked Green line (~96 km), vertical1610Direction 1 electric field (eastward)E1Nu Ne Ni Te Ti Tr Vi32_3304Nu72_6121Vn1Direction 1 Neutral wind (eastward)1411Variation in elevation (end El-beg El)145El ChangeFeeElectron energy flux21309618h Vnn Amp8-h northward neutral wind amplitude3309NNRSWPMLH Number noise gates in radar sweepNu Ne Ni Te Ti Vi71_720841_4207Ne Te Ti Vi109Additional increment to max altMax Alt IncZ GSM294Z Coord Geocentric Solar MagnetosphericNe Te Ti Faraday rot data 1966-1969 (Te>Ti forced)10_30003ERROR FOR Temperature ratio (Te/Ti)error Te/Ti-570ACFrn22Normalized real ACF at lag 223822Number of coefficients in analysisNo Coeffs9213916ACFin16Normalized imaginary ACF at lag 16Nu Ne Ni Te Ti Vi71_7112Normalized imaginary ACF at lag 11ACFin113911error MLH par 21-3320ERROR FOR MLH parameter 21Nu Ne Ni Te Ti Vi CF73_6208Vn41440Direction 4 Neutral wind (perp east)SON Begin month/day of composite (UT)Beg mmdd353573_6120Nu Ne Ni Te Ti Vi CFSt. Santin data quality code 1STS Dat QC1466lg(BkgNois)Log10 (background noise, residual)2560mmdd anal25Month/day (UT) of analysis date-660ERROR FOR Ion Composition - [H+]/Neerror [H+]/Ne[HE+]/NeIon Composition - [HE+]/Ne6505140_17002Tn Em VnDst hourly gnd magnetic index in nT212_30006Interplanetary Mag Field Bx GSM2204Bx GSMap index (3-hourly)ap335Vn tides mean and semi-diurnal (sd)1320_17001Ne Te Ti Tr Vi20_300093900ACFsf0Scale factor for ACF at zero lagGeomagnetic field strengthBmag210Vn tides LTCS period analysis1240_179995020_17002Vn 1994-1998 cubic spline fitsVn 30-min winds1310_17001366Estimated Hemispheric Power IndexHem PwrIndx1010Geographic unit vector rotation angleRot angl-gg111Alt IncAdditional increment to altitudelog10 (Fe number density)905lg([Fe])10_1050ViPrecision Solar Photometric TelescopePSPT_MLSOH20_2001Nu Ne Ni Ti Tr ViERROR FOR Height of maximum electron density-540error Ht Max Ne9608h Vne Amp8-h eastward neutral wind amplitudeNu Ne Ni Te Ti Vi CF73_61122521Ch1 CalChannel 1 Calibration (cnt/s over R)ACFrn24Normalized real ACF at lag 243824Mean upward neutral windMean Vnu93472_6207Nuerror Vn3ERROR FOR Direction 3 Neutral wind (up)-1431928Vnu residUpwd Residual Sqrt[1/N*sum(wi-wf)**2]log10 (uncorrected electron density)lg(RawNe)505ERROR FOR SON Correction term = Ux-Vxerror uxcorr-3585DVnn/Dx/mkm4057AFP QC D(Vnn)/Dy per 1000 km (y +Nwrd)siguytot3590SON Total error on Uy-950ERROR FOR 12-h eastward neutral wind amplitudeerror 12h Vne Amp2-dy northward neutrl wind amplitude2dy Vnn Amp971JRO E beam log10(1+RxC incoh. pwr/noise)3105PwrI RxC E1282Direction 8 Ion velocityVi8Relative neutral temperature813relativ Tnlg(NoisPwr)4004PKR QC log10 (noise pwr in spectrm)Ne20_3000242Local solar time diff (=SLT-UT) +E lonSLT-UTNe Ni Te Ti Tr Tn Vi50_5121log10 (joule energy spec. heat rate)lg(Qjoulv)2121SP4D_StokesIStokesIStokes I Polarization ParameterNe Te Ti Vi40_4204-3626ERROR FOR SON Vector Velocity Magnitude (XY plane)error XY |Vel.|AFP Et Th4052AFP QC Etalon ThicknessSON Correction term = Ux-Vx3585uxcorr72_6502Nu Ne Ni Te Ti Vi CF2210IMF BInterplanetary Mag Field strength6320_17002Na Tn nightly means-4022ERROR FOR CSL QC Neutral temperature looking Eerror CSL TngE72UT of Moonset (from US Naval Obs)TmoonsetLn int J4Line int (1 hemi): dir 4 current den1940Rec Delay496Receiver delay timeHecht 4ch Ph. 1=moon down; 0=moonlitH4P Moonflg4103MLH Number calibration samples in prof3304NCSAMP24-h max upward neutral wind phase24h Vnu Phs987ACFin203920Normalized imaginary ACF at lag 2020_30016Nu Ne-710error Col FreqERROR FOR Ion-neutral collision frequencyVi861_7001PACE Az230PACE magnetic azimuthlg(Nn)840log10 (neutral number density)EceCharacteristic electron energy2157Nu Ne Ni Te Ti Vi CF72_6310Na Tn Vn los nightly means6320_17012Nu Ne Ni Te Ti Vi CF72_6206CSL TngE4022CSL QC Neutral temperature looking EJRO W beam log10(1+RxA coher. pwr/noise)3102PwrC RxA W24-h max northwrd neutral wind phase24h Vnn Phs9462501lg(Bright)log10 (line/band brightness)2573Ch3 Bkg CorChannel 3 Background correction3586uycorrSON Correction term = Uy-Vy74_6712Nu Ne Ni Te Ti Vi CFNormalized real ACF at lag 26ACFrn263826-3600ERROR FOR SON Direction 5 F Region ion velocityerror Vi5FF10.7a(Sa)F10.7 Multiday average352AQF QC Standard deviation in 142140621421 s devERROR FOR Height integral pedersen conductivity-2040error HtInt Ped Cerror Vi8ERROR FOR Direction 8 Ion velocity-128095_30101Ne Ti Tr ViTn5700_17031SON CW angle from GM North for 3628-XYEF nangle36298h Tn Phs8-h max neutral temperature phase967Den srcSON Source of density profile3505ERROR FOR Line of sight neutral vel (pos = away)-803error VnlosSON Cross correlation coefficient Uxy3576xccof UxyACFrn19Normalized real ACF at lag 193819170_8015none401Lag1Lag to the first range gateEf Ep Qp Sg NH for several AMIE campaigns311_30021E2Direction 2 electric field (northward)1620error 24h Vne Phs-945ERROR FOR 24-h max eastward neutral wind phaseNu74_6711Tn5720_1700130_13211Vi Vn LTCS E regionCHT/SON QC1471Chatanika/Sondrestrom data qual code 1Vn tides LTCS period analysis1220_1799941_4205Ne Ni Te Ti Vierror J5ERROR FOR Direction 5 electric current density-1850-1840error J4ERROR FOR Direction 4 electric current density1430Vn3Direction 3 Neutral wind (up)Nu80_9006Ion Velocity spread (spectral width)Vi Spread585Smpl RngNumber of samples in range ave114Ne50_5102Nu Ne Ni Te Ti Vi71_731241_4206Ne Te Ti ViJicamarca data quality code 1JRO Dat QC1451Ht Max NeHeight of maximum electron density54012h Vnu Amp98812-h upward neutral wind amplitudeerror Vi5-1252ERROR FOR Direction 5 Ion velocity (perp north)Electron densityNe512Vn tides 4-day CEDAR/TIMED analysis1270_17100Nu Ne Ni Te Ti Vi71_7306Particle (el. and pos. ion) energy fluxFepart2136Vn hrly aves, combined E/N winds1140_20004Vn11412Direction 1 Neutral wind (eastward)72_6714Nu Ne Ni Te Ti Vi CF156Reference geodetic longitudeRef Gd LonVn2Direction 2 Neutral wind (northward)1421ACFrn13Normalized real ACF at lag 133813310_11032Tn Vn Ep tides 30kV-905error lg([Fe])ERROR FOR log10 (Fe number density)OPeNDAP DAS (Data Attribute Structure) data fileDASOPeNDAP DDX (Data descriptor in XML) data fileOPeNDAP DDX (Data descriptor in XML) data fileDDX5700_17042TnNu Ne Ni Te Ti Vi CF71_630671_7000Nu Ne Ni Te Ti Vi CFTime > 0UT36Time past 0000 UT72_6120Nu Ne Ni Te Ti Vi CFJicamarca data quality code 4455JRO Dat QC5Tsys IncAdditional increment to system temp483PFQC4001PKR QC 0=OkayVi Ef Viperp(ht,mlat), Vipar=080_15610Ch2 Cal2522Channel 2 Calibration (cnt/s over R)2139Particle energy heat rate height int.QparthNu Ne Ni Te Ti Vi72_7210VbiasSON Amount subtracted from Vlos3567IMF1 S/C B4121IMF 1min S/C B: Bx!Vx IDx IDyz32_3071Nu Ne Ni Te Ti Tr Vi352's avg code: 1=>81day ; 2=13mon353352 Avg TypRelBkgRadncRelative background radiance2555Vn1560_1700230_3302Nu Ne Te Ti Tr ViERROR FOR 24-h ion temperature amplitudeerror 24h Ti Amp-94428Beginning hour/min (universal time)Beg hhmm3521Elm pos 2SON Mean elevation position 21221Vi2(F)Direction 2 F-region ion velocityNu Ne Ni Te Ti Vi CF73_6312UT of Nautical sunrise (szen=102 deg)77Tsris NautHall conductivity2020Hall Cond5160_17011Em Vn vertical meas in zero vel ref357356 Avg Typ356's avg code: 1=>81day ; 2=13monSTS Dat QC4469St. Santin data quality code 4Vn derived data from kindat 70015340_1700172_7502Nu Ne Ni Te Ti ViMLH parameter 46MLH par 463345-1455error Vn5hERROR FOR Direction 5 Neutral wind horizontl comp4470_18001Ne Nn Strickland transport model inputs890log10 (HE number density)lg([HE])Au Index (hourly mean)326Au (hr)SON End centisecond of composite (UT)End csec35412514Ch1 BrightChannel 4 line/band brightnessEastward component of geomagnetic field206BeLn int J5Line int (1 hemi): dir 5 current den1950Vn tides hourly winds1320_17002Ef Je Sg80_15620Vi1(F)1211Direction 1 F-region ion velocityDirection 10 Elevation angle1090El(dir 10)Nu Ne Te Ti Tr Vi32_3301901log10 (NO number density)lg([NO])830_7001ViNo. samples in dir. 3 avg. (upward)NoSmpl Dir3424EHP median estim. Electron Hp inputEHP med HPe4161Int Time61Integration time for these dataAu Index (1 or 2.5 min sample)322AuNormalized real ACF at lag 8ACFrn83808ERROR FOR 12-h northward neutrl wind amplitudeerror 12h Vnn Amp-95197End of event flag (0=off, 1=on)End pos flgNe Ti Tr Vi95_30110IDLIDL Script Data FileVn monthly quiet-time averages5140_17001IMF1 S/CposIMF 1min S/C Pos: !IMF IDx IDyz4123UT of Civil sunrise (szen=96 deg)Tsris Civil75OPeNDAPOPeNDAP data fileNu Ne Ni Te Ti Vi CF74_6714Geomagnetic IndexKp: high geomagnetic activity9.0High geomagnetic activity (as measured by index Kp)9.0Medium geomagnetic activity (as measured by index Kp)Kp: medium geomagnetic activity3.03.0Kp: low geomagnetic activityLow geomagnetic activity (as measured by index Kp)Kp IndexKp310Vi Ef Je Qj Qp Sg80_150213301Power NrmKMLH Power Normalization constant80_5152NeIon Composition - [O+]/Ne[O+]/Ne620-1411ERROR FOR Direction 1 Neutral wind (eastward)error Vn110YrYear (universal time)Normalized imaginary ACF at lag 253925ACFin25900lg([H])log10 (H number density)3800ACFrs0Scaled real ACF at zero lag935Mean VneMean eastward neutral windTi Vn tides LTCS80_15999JRO Dat QC3453Jicamarca data quality code 3Neutral temperatureTn181250_15115Nn Tn Vi Vn Ef pre-LTCSR Dop FoffReceived doppler frequency offset49212h Ti Amp12-h ion temperature amplitude954Brightline/band brightness2502Normalized imaginary ACF at lag 173917ACFin17SON Total error on Ux3589siguxtot73_6116Nu Ne Ni Te Ti Vi CFAl Index (hourly mean)Al (hr)325ERROR FOR Direction 7 Ion velocityerror Vi7-127211_1850Ne Bistatic daytime E-region-412ERROR FOR log10 (signal to noise ratio)error lg(S/N)72_6208Nu Ne Ni Te Ti Vi CF30_3304Nu Ne Ni Te Ti Tr Vi1275_17100Vn tides 4-day CEDAR/TIMED analysislg(avgRale)UIL QC log10 (av Rayleigh) = NrmlzFctr4018SON Total error on Uzum (code 1460)siguztot3584No Smpl usdNo samples used419Apex Lon246Apex longitude in measurement volumeTn Vn Ep 30kV310_1103172_7112Nu Ne Ni Te Ti Vi3810Normalized real ACF at lag 10ACFrn10Vi80_15520117Virtual heightVirt Ht535log10 (max Ne in m-3)lg(MaxNe)ACFrn273827Normalized real ACF at lag 27AFP QC Free spectral range(arb p unit)4051AFP SpctRngDirection 9 Ion velocity1290Vi91620_17021Vn tides normal analysis94224h Tn Amp24-h neutral temperature amplitude72_7000Nu Ne Ni Te Ti Vi CF72_7310Nu Ne Ni Te Ti ViVnlos802Line of sight neutral vel (pos = away)1241Direction 4 Ion velocity (perp east)Vi4-4003ERROR FOR PKR QC Avg of Galactic Noiseerror PF Gal Nois311_30011Ef Ep Qp Sg old NH 23-26 Sep 198672_6210Nu Ne Ni Te Ti Vi CFHecht 4ch Ph. 1=good night, 0=so-so4104H4P nitflg474Res. Vel. Pairing CodeRV Pair CD94124-h northwrd neutral wind amplitude24h Vnn AmpNe Ni Te Ti Vi CF45_8038Binc216Geomagnetic field downward inclinationVi Bisect590Bisector ion vel (bistatic sys,pos=up)-1260error Vi6ERROR FOR Direction 6 Ion velocity (antiparallel)Vn tides Groves coefs, normal anal1620_1701180_5100Ne610Velocity direction - local elevationVel ElNu Ne Ni Te Ti Tr Vi31_3304Apex LatApex latitude in measurement volume226Int TimeIntegration time for these data624164EHP original estim. Ion Hp inputEHP origHpi20_12999Ti Vn tides LTCSTn Vn Ep 90kV310_11091AreciboThe Arecibo Observatory is located in Arecibo, Puerto Rico on the north coast of the island. It is operated by Cornell University under cooperative agreement with the National Science Foundation. The observatory works as the National Astronomy and Ionosphere Center (NAIC) although both names are officially used to refer to it.
The observatory's radio telescope is the largest single-aperture telescope ever to be constructed. (Compare "multiple aperture telescope".) It collects radio astronomy, terrestrial aeronomy, and planetary radar data for scientists around the world. Usage of the telescope is gained by submitting proposals to an independent board of referees.
Although it has been given many usages, the observatory's main purpose is to detail and observe stellar objects.http://en.wikipedia.org/wiki/Arecibo_Observatoryhttp://www.naic.edu/Direction 7 Ion velocity1270Vi7484Calibration temperatureCal TempMonth/day (universal time)20mmdd8h Tn Amp9628-h neutral temperature amp80_5124Te TiTn Em VnInsert here description of the 5430/7001 operating mode5430_7001ACFrn163816Normalized real ACF at lag 1629Beg TimeIncBeginning additional increment to hhmmVi835_7001ERROR FOR 12-h ion temperature amplitudeerror 12h Ti Amp-954Direction 4 electric current density1840J473_6122Nu Ne Ni Te Ti Vi CFerror Umerid-3582ERROR FOR SON Horizontal magn neutral windSON Begin year of composite (UT)Beg yr comp3534ACFin14Normalized imaginary ACF at lag 14391494524h Vne Phs24-h max eastward neutral wind phaseMLH par 533352MLH parameter 53Nu Ne Ni Te Ti Vi73_7312XY |Vel.|3626SON Vector Velocity Magnitude (XY plane)2495log10 (Rayleigh counts)lg(RaylCnt)JRO E beam log10(1+RxC coher. pwr/noise)PwrC RxC E3106UparSON Portion of Umerid due to Vpar3512TeElectron temperature5605700_17001TnRFP median nightly zero los windRFP mdlos041713628SON E Field Magnitude (XY plane)XY |EF|Tn Em3010_17001PC Pot Dif2301Polar cap potential differenceBz GSMInterplanetary Mag Field Bz GSM2208error UparERROR FOR SON Portion of Umerid due to Vpar-3512Lin Int Ne522Line integrated electron densitylog10 (Pedersen Conductivity)lg(Pd Cond)2011Year (UT) of analysis dateYr anal15Nu Ne Ni Te Ti Vi71_7402433Cod typeCode type (0=non,1=cmplmntry)31_3408Nu Ni Ti Tr Vi2200_17999Vn tides LTCS period analysisEf Je Sg80_1562120_2015Ne32_13022Ti tides LTCS40_4201Ne Te Ti ViTn nightly means 87+/-1.85 km6320_17087error MLH par 53-3352ERROR FOR MLH parameter 53Nu Ne Ni Te Ti Tr Vi32_330280_15023Vi Ef Je Qj Qp SgHeight integral pedersen conductivity2040HtInt Ped C3502SON EPEC F-Region source codeF SrcTn Em Vn [OH] line (~87 km, cardinal dirs5060_17004Raw Ne Inc501Uncorrected electron density increment413Smpl T AvalNo samples available in time averageNu Ne Ni Te Ti Vi CF73_6502Tn Em Vn5460_17001Insert here description of the 5430/17001 operating modeMLH parameter 243323MLH par 245340_7002Tn Em Vn combined meas in zero vel ref-1940ERROR FOR Line int (1 hemi): dir 4 current denerror Ln int J4Vn derived data from kindat 70025340_17002153Ref Gd LatReference geod latitude (N hemi=pos)LinEmisRat2507Relative line emission rate72_6999NuERROR FOR 2-dy northward neutrl wind amplitude-971error 2dy Vnn AmpJRO normalizing factor (JRO661111A)3100T Norm Fctr296Y GSEY Coordinate Geocentric Solar EclipticVn tides d/sd func(altitude)1320_17003Ne Ti Tr Vi95_30201TsysSystem temperature482log10 (Hall Conductivity)lg(Hl Cond)2021SON Cross correlatn on Une from signeutxccof Uenn358080_15525Ne Te TiRadiative transfer source functionsp4d_sourcefunctionSBZERO355F10.7qF10.7 solar flux qualifier observed72_6117Nuerror TnERROR FOR Neutral temperature-8109916-h northward neutral wind amplitude6h Vnn AmpTn Vn tides320_20001AE (AU,AL,AO) gnd magnetic index (1m,hrly)211_300081140The Poker Flat MST radar was located at the Poker Flat Rocket range about 200 m above mean sea level in Alaska at (65.13N, 145.46W), and operated between 1979 and 1987. The last 2 years are not in the CEDAR Data Base. The inclination angle is about 77 degrees, and the declination is about 29 degrees to the east of north.
The Poker Flat radar was a high power radar, with three narrow beams. One beam looked vertically (kindat=20003) and the other two were inclined at 15 degrees to vertical, or at an elevation angle of 75 degrees. The 'east' beam had an azimuth 26 degrees north of east (kindat=20001) while the 'north' beam had an azimuth 26 degrees west of north (kindat=20002). Most of the data were taken using all three beams but some, especially in the early days, were taken with only the vertical beam or with only the oblique beams. During an experiment one or more beams were sometimes inactivated. The cycle time for a complete set of vertical and oblique records seldom exceeded 10 min and was typically 1 min. When available, velocity measurements from the two oblique beams were combined to give eastward and northward components of the neutral wind (kindat=20004). The velocity spread is twice the square root of the second moment of the power spectrum and is a measure of shear or turbulence in the measurement volume.
Data quality below 5 km is definitely dubious and below 8 km should be treated with suspicion due to recovery problems. The more obviously false data have been removed from this data set but consistently false data are hard to distinguish from the real thing and may be included.
The original Poker Flat data set has been subjected to an extensive set of checks to remove various interference modes, outliers and otherwise non-atmoshperic data. The parameters for the remaining data have been averaged for all appropriate records that commenced within a one hour interval. Note that these are averages of the derived parameters and not parameters derived from an average velocity spectrum.
In the absence of any signal echo the main contribution to noise is the radio noise from our galaxy. Hence there is a siderial variation (of about 4 db) in the noise level. Atmospheric absorption events reduce the level of noise. Receiver gain and cable attenuation fluctuations may have a small influence. Operator modification of gain controls are rare. Strong signals can corrupt the computation through their sidelobes. The errors given are the root mean square values of the deviation from the mean for that hour. PKRhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pkrPoker Flat Alaska MST RadarCEDAR1040ARMThe ST (strato/troposphere) radar at the National Astronomy and Ionosphere Center (NAIC) at Arecibo, Puerto Rico (18.3N, 66.75W), made measurements during the AIDA (Arecibo Initiative in Dynamics of the Atmosphere) campaign of March-May, 1989, an international multi-instrument campaign which was conducted to compare wind measurements in the mesosphere taken by various radar and optical devices. The tropo- and stratosphere data taken by the Arecibo ST radar during this period were largely decoupled from the main objectives and the observations of the other instruments. Data are available for both day and night times. Integration time per profile varies and is on the order of 30 sec to 1 min. However, because the mesosphere observations were interleaved with this data set, there are many gaps between profiles on the order of a few minutes. During AIDA, the altitude range sampled was from about 5 to 20 km, and the resolution was about 0.3 km. For this data set, the antenna azimuth scan pattern was very roughly as follows: 1.5 hrs at 14 or 32 deg, 10 min at -76 or -58 deg, 10 min at 194 or 212 deg, 30 min at 104 or 122 deg, 10 min at 194 or 212 deg, and 10 min at -76 or -58 deg, then repeat. Beware that the times do appear to vary. Elevation angle was fixed at about 79 degrees. Results from AIDA have been published in J. Atmos. Terr. Phys., 55, 1993, a special issue dedicated to the campaign. H. Mario Ierkic was responsible for the operation of the Arecibo ST radar during AIDA, and John Cho put this data set into the CEDAR Data Base.
This program extracts the following data from the Doppler spectra of the Arecibo ST radar: (1) Line-of-sight velocity of the clear air, (2) signal spectral width, and (3) SNR. Item (1) is self-explanatory. Items (2) and (3) yield information about the actual radar scattering mechanism. If the mechanism is turbulence, then (1) and (3) yield the turbulence intensity. For further information see Gage and Balsley [1980]. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:armArecibo P.R. MST Radar33http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mlhThe incoherent scatter transmitter station at Millstone Hill, Massachusetts (42.6N, 71.5W) has been in operation since 1960. The facility is part of and operated by the Massachusetts Institute of Technology.
ISR data comes from the fixed zenith antenna, the steerable antenna, or both.
The electron densities from the power profile were calibrated with an on-site ionosonde, where recently, this ionosonde has been the University of Massachusetts at Lowell digisonde. Since the Coast Guard uses some of the frequencies needed to properly scan the ionosphere, calibration can sometimes be difficult. The calibrated electron density is then corrected for Te and Ti effects, where Te and Ti come from auto-correlation fits. The calibration and auto-correlation fits now have the same height resolution, although in the past, the auto-correlation fits had lower height resolution.
The ion composition changes from mostly O2+ and NO+ at lower altitudes, to mostly O+, and then to H+ and some He+ at higher altitudes. Above 400 km, the percent H+ is computed along with the major ion O+. At lower altitudes, the ratio of molecular ions to the total number of ions is modeled as specified by the FORTRAN code segment below.
REAL FUNCTION PMF(Z)
Z1=AMIN1(-(Z-120.)/40.,50.)
H=10.-6.*EXP(Z1)
Z2=AMIN1(-(Z-180.)/H, 50.)MLH33Millstone Hill: steerable L-band ant.The Obninsk, Russia (55.11N, 36.51E; ~172 m above msl) 33.3 MHz meteor radar has been in operation since 1964. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (51.2, 111.0) degrees. The magnetic inclination and declination angles were 70.5 deg and 8.3 deg. The magnetic local time at 0 Universal Time (UT) is about 0219 MLT. The solar local time (SLT) is UT plus 2 hours and 26 minutes (36.51/15=2.434). With no height ranging, the observations come approximately from 95 km.Obninsk Russia Meteor Wind Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltr1750OBN31Millstone Hill: steerable UHF antennahttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mlhMLH31The incoherent scatter transmitter station at Millstone Hill, Massachusetts (42.6N, 71.5W) has been in operation since 1960. The facility is part of and operated by the Massachusetts Institute of Technology.
ISR data comes from the fixed zenith antenna, the steerable antenna, or both.
The electron densities from the power profile were calibrated with an on-site ionosonde, where recently, this ionosonde has been the University of Massachusetts at Lowell digisonde. Since the Coast Guard uses some of the frequencies needed to properly scan the ionosphere, calibration can sometimes be difficult. The calibrated electron density is then corrected for Te and Ti effects, where Te and Ti come from auto-correlation fits. The calibration and auto-correlation fits now have the same height resolution, although in the past, the auto-correlation fits had lower height resolution.
The ion composition changes from mostly O2+ and NO+ at lower altitudes, to mostly O+, and then to H+ and some He+ at higher altitudes. Above 400 km, the percent H+ is computed along with the major ion O+. At lower altitudes, the ratio of molecular ions to the total number of ions is modeled as specified by the FORTRAN code segment below.
REAL FUNCTION PMF(Z)
Z1=AMIN1(-(Z-120.)/40.,50.)
H=10.-6.*EXP(Z1)
Z2=AMIN1(-(Z-180.)/H, 50.)
Davis, Antarctica MF radarDAVThe Davis, Antarctica (68.60S, 77.97E; ~1 m alt) 1.94 MHz MF radar has been in operation since April 1994. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (64.1, 152.4) degrees. The magnetic inclination and declination angles were 81.7 deg and 21.7 deg. The magnetic local time at 0 Universal Time (UT) is about 0505 MLT. The solar local time (SLT) is UT plus 5 hours and 12 minutes (77.97/15.=5.198). Code 42 (LST-UT) was corrected from 1.E-03 hr to hhmm in Sep 2004.
The original data files are hourly averages of the zonal and meridional velocity in Local Time (LT), which is 5 hours later than UT. Smaples are taken every 2 min, so a possible 30 samples can be had between 05:00:00 LT and 06:00:00 LT. The midpoint is 05:30:00 LT or 0:30:00 UT, or 5:42:00 SLT. Local times have been converted to the mid-point SLT, or 42 min (0.618 hr) are added to the beginning LT hour.
The MF operating frequency is 1.94 MHz, with a peak transmitter power of 25 kW, 40 kW starting in 2004. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 and 25 millisec, respectively during the day and night. There are usually 32 coherent integrations during the day and 16 at night, using 256 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, want about 2 min or 102.4 sec integration day or night, or 12.5x10-3sec * 32 integ * 256 samples = 102.4 sec and 25x10-3sec * 16 integ * 256 samples = 102.4 sec.]
The height coverage is 50-100 km during the day or night at Davis. The pulse width is 30 microsec, giving a height resolution of 4.5 km assuming a simple rectangular wave pulse [range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 30x10-6s / 2 = 4.5 km]. However, the height range provided is every 2 km between 50 and 100 km starting in 2003, and 50 and 98 km earlier. 1215http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dav175The total hemispheric power input is computed from NOAA/TIROS and DMSP satellite measurements of high latitude precipitating energy flux carried by ions and electons with energies between 300 eV and 20 keV (NOAA/TIROS), or carried by electrons with energies between 460 eV and 30 keV (DMSP). The satellite orbits are sun synchronous around 850 km altitude. Times given are the center of the polar pass used to make the estimate where a typical polar pass takes about 25 minutes. Often there are two satellites operating simultaneously providing coverage at 30 to 60 minute intervals between auroral latitude crossings. The energy flux observations made during a single pass over the polar regions (above about 45 degrees of magnetic latitude) are used to estimate the total precipitating power input to a single hemisphere at that time. This power index was devised by David Evans for the NOAA/TIROS satellites, and adapted for the DMSP satellites by Frederick Rich and William Denig.EHPhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ehpEstimated Hemispheric PowerRFPResolute Bay Fabry-Perot Interf Sp5535The Fabry-Perot Interferometer at Resolute Bay, Canada (74.73N, -94.89E, 87 m ASL) has been operated since 2003 by the High Altitude Observatory of the National Center For Atmospheric Research. The apex magnetic coordinates of Resolute Bay at 250 km height in 2004 were (83.1, -39.0) with a magnetic declination of -24.4 deg, an inclination of 88.0 deg, and 0 UT at 16.31 MLT.
The dispersing element of the interferometer is an air-spaced, 10 cm diameter effective clear-aperture Fabry-Perot etalon. It has a fixed gap of 2.0 cm. The etalon is housed in a temperature controlled chamber (Wu et al. 2004). The instrument detector is a back illuminated CCD camera with 1024x1024 pixels and 1x1 inch size. The CCD temperature is set at -55 C. The readout noise of the CCD is 4 electrons.
The interferometer has an 8-position filter wheel. The wavelengths used at Resolute Bay are:
1. The red line (630.0 nm, kindat=17001) of atomic oxygen (OI) with a typical emission height peak in the range 210 to 300 km.
2. The green line (557.7 nm, kindat=17002) of atomic oxygen (OI), with a typical emission height peak range near 94-98 km.
3. The [OH] line (892.0 nm, kindat=17003) of the nightglow excited hydroxyl [OH*] with an emission peak between about 87 and 91 km. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:rfphttp://cedarweb.hao.ucar.edu/0.0GPS1100.0Global Positioning System ReceiversGlobal Positioning System ReceiversAMIE Model OutputAREThe Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure is an NCAR model. A subset of the list of AMIE campaigns has been put into the CEDAR Database. These campaigns are:
* 18-19 January 1984
* 23-26 September 1986
* 12-16 January 1988
* 20-21 March 1990
* 8-9 November 1991
* 27-29 January 1992
* 28-29 March 1992
* 20-21 July 1992
Most of these campaigns do not have plots on the CEDAR Database. But the input Goose Bay and Halley HF ion drifts are available for some of these campaigns.311http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:arehttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aeiAEIThe CEDAR Database contains 1 min and hourly values of the magnetic indices AE, AL AU and AO from 1 January 1978 to 30 June 1988, and provisional AE indices from 1 January 1990 to 31 December 1994. The provisional AE indices came from http://swdcdb.kugi.kyoto-u.ac.jp/aedir, where one can get recent estimated AE plots also. The older AE came from World Data Center in Boulder where one can get:
* hourly AE, AL, AU, AO (1 July 1957 - 30 June 1988)
* 1 min AE, AL, AU, AO (1 Jan 1986 - 30 June 1988). Previous years of 1 min data must be ordered from NGDC, or taken from the CEDAR Database.
When the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure uses ground magnetometers, it can calculate the AE at usually 5 minute intervals. AE is thus usually available for the list of AMIE campaigns.211Geophysical indices from NGDC: AEThese are model lunar semidiurnal tides calculated in the Earth's atmosphere. The lunar day is 24 hr 50.47 min. The phases vary between 0.00 and 12.00 hours in lunar time, where 0 lunar time refers to the time of lower transit. This is when the moon is 180 degrees opposite one's position on Earth, and is entirely analogous to solar local time. The calculations were done for each month, where the day assumed was the 15th of each month. The results are independent of solar cycle, so the year is arbitrary. The year 1993 was chosen because this was the year that the model runs were made. The semidiurnal amplitudes and phases of the eastward neutral wind, the northward neutral wind, the neutral temperature, and the geopotential are given for 12 altitudes between about 78 and 102 km. The altitudes are slightly for each month. The original results were southward winds, so the phases were shifted by 6 hours to make them northward. The maximum amplitudes are just below 20 m/s for the winds, about 6 degrees K for the temperature, and nearly 2500 m2/s2 in geopotential. Some temperature amplitudes are shown as 0 near the pole but with some phase. This is the result of truncating amplitudes less than 0.005 K.SDLhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sdl321Vial/Forbes Model Lunar TidesThe incoherent scatter transmitter station at St. Santin, France (44.6N, 2.2E) operated between 1963 and 1987. The CEDAR Data Base holds all the data taken from 1966 until the end. Up until June 1973 and after July of 1986, the only receiver station operating was located at Nancay (47.4N, 2.2E). Between 1973 and 1986, 2 other receivers also operated at Montpazier (44.7N, 0.8E) and at Mende (44.5N, 3.45E).
In general, the daytime height range is 105 to 350 km, while the nighttime height range is 200 to 500 km. Before January 1, 1969, the faraday correction is not taken into account in the computation. The spectrum are analysed following the scheme described in Waldteufel (1970). The ion drift component is quasi parallel to the magnetic field as measured by the Nancay receiving station. Because the transmitter is not located at the receiving location, the bisector velocity is plotted for the period when only Nancay data were received. When all 3 receivers were on, then the data are 30 minute averages and the ion drifts in the geomagnetic coordinate system are calculated.
There are 4 areas in the summary plots. There are image plots as a function of height and time of the electron density, electron temperature, and ion temperature. Bin sizes are 40 minutes in time and 40 km in height. For the Nancay period alone there is also an image plot of the bisector velocity, while this is replaced by line plots of the ion drift in the perpendicular east, north and parallel directions at the altitude closest to 300 km. when there are 3 receivers.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:stsSaint Santin: Nancay receiverSTS414110JROThe 50 MHz incoherent scatter radar at Jicamarca, Peru (11.95 S, 76.87 W; 520 m alt) has been operating since 1963. On day 359 of 2001 at the ground, the apex magnetic lat,lon were (0.58, -5.12) deg. The magnetic inclination and declination angles were 1.145 deg and 0.367 deg. The magnetic local time at 0 UT is ~1835 MLT.
There are three basic types of operating modes for the incoherent scatter radar:
1. Faraday rotation to obtain electron densities (Ne) and electron (Te) and ion temperatures (Ti)
2. the drift mode
3. the bistatic coherent radar mode (E-region Ne above Paracas)
The drift mode, which finds perpendicular east and north (near vertical) ion drifts, has data from 1984 to the present. The analysis scheme to derive the drifts was changed starting in September of 1994 with a resulting increase in the data quality. Hard copies of time series plots of the older ion drifts are available upon request from NCAR.
The bistatic coherent radar experiment involves the 50 MHz transmitter at Jicamarca and a reciever at Paracas (13.85 S, 76.25 W), which is about 200 km south of Jicamarca. E region (~95-110 km) electron density data are available using a 4 microsecond (~0.6 km) pulse length from Mar 2004. This experiment can run concurrently with either the Faraday rotation or the drift mode. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:jroJicamarca Peru I.S. Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:y4pThe Aerospace 4 channel filter photometer at Fort Yukon, Alaska (66.57N, 214.73E) was developed to estimate the energy flux of auroral electrons, their average energy Eo (usually from 0.1 to 30 keV using a modified Gaussian or Maxwellian shape), and a scale factor fo for the atomic oxygen densities [O] from an MSIS model atmosphere. The [O] densities using the scaling factor fo can be compared to GUVI/TIMED estimates. The technique is only valid for clear night conditions where the solar zenith angle (sza) is greater than 102 deg (code 4102=1), and there is enough auroral emission (427.8 nm brightness, code 2421). Fort Yukon apex magnetic coordinates are (67.3, -94.7) at 110 km in 2001, with 0 UT corresponding to 12:36 MLT. The magnetic inclination and declination angles are 78.7 deg and 25.6 deg. The photometer looks up the magnetic field line with a field of view (fov) of about 1 deg. The data rate can be programmed, but typically each channel is integrated for 1 sec, where the whole cycle including filter moves takes about 8 sec.
The 4 channels correspond to:
1. N2+ (427.8 nm, blue) first negative group (1NG) 0,1 molecular band
2. OI (630.0 nm, red) forbidden
3. OI (844.6 nm, eight) permitted
4. N2 (871.0 nm or 871.4 nm) first positive group (1PG) 2,1 molecular band Fort Yukon Alaska 4 Channel Photometer4473Y4PSaskatoon HF Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:shf861The Saskatoon HF radar is located in central Saskatchewan (52.16 deg N, -106.53 deg E) and looks over a section of ionosphere poleward of 53 deg N that covers north-central Canada including Hudson Bay and the Canadian arctic archipelago. It has operated since 1993. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Saskatoon velocity data is located at Kapuskasing, Canada.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 23.1 deg E of N. SHFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:julJULIA Jicamarca Peru Coherent RadarJUL840For the JULIA coherent scatter radar: The Jicamarca Radio Observatory is a facility of the Instituto Geofisico del Peru and is operated with support from the National Science Foundation Cooperative Agreement ATM-0432565 through Cornell University.
These data are proxy measurements of F-region ExB ion drifts derived from the 150-km echoes measured with the Jicamarca (11.95 S, 76.87 W; 520 m alt) Unattended Long-Term studies of the Ionosphere and Atmosphere (JULIA) system. On day 359 of 2001 at the ground, the apex magnetic lat,lon were (0.58,-5.12) deg. The magnetic inclination and declination angles were 1.145 deg and 0.367 deg. The magnetic local time at 0 UT is ~1835 MLT.
Jicamarca is the site of a 50 MHz incoherent scatter radar (ISR, kinst=10) in operation since the 1960s. The JULIA system is a coherent scatter radar (kinst=840) that uses two low-power 50 MHz transmitters which are phased together to excite the transmission antennas as a single unit. The JULIA system was intended for uninterrupted observations of ionospheric and atmospheric irregularities. JULIA shares the antenna, receiving system, processing, etc. with the ISR, but uses different transmitters. The coherent and incoherent scatter radar transmitters can operate at the same time for intercomparisons [e.g. Chau and Woodman, 2004].
The JULIA data are divided into 3 categories based on their altitude range and local time of occurrance. Observations of the E region electrojet (EEJ) are made between altitudes of 85 and 140 km in the morning and evening. The equatorial spread F (ESF) region irregularities are sampled between 95 and more than 850 km at night. For the valley region and so-called "150 kilometer" echoes, altitudes between 130 and 180 km are sampled during the day. The present 150-km echoes are averages between 140 and 170 km.
JULIA ionospheric irregularity data have been collected beginning in August 1996. Signal-to-noise ratios are shown as intensities. Horizontal zonal drifts are deduced with radar intererometry. Vertical drifts refer to Doppler phase speeds where positive values imply upward phase propagation in the EEJ and ESF modes.
Echoes from 150-km irregularities were first observed in the early 1960's over Jicamarca using the ISR [Balsley, 1964]. These echoes occurr only during the daytime and show very little seasonal dependence. The 150-km echoes have been observed at Jicamarca with the ISR on a campaign basis [e. g., Kudeki and Fawcett, 1993]. Sucessful low power observations of 150-km echoes have been performed since 2001 with the JULIA radar using two different antenna beam configurations (a single vertical beam, and an east-west beam pair). Using the vertical beam, only the vertical ion Doppler velocities are obtained, while using the east-west beam position both the vertical and zonal ion velocities are measured. In the latter case, two beams are used at the same time using diffent antenna sections.
An important finding from the study of these 150-km echoes is that the daytime vertical Doppler velocities of the 150-km irregularities averaged over the altitudinal region of the irregularities were in excellent agreement with the mean F region (200-500 km) ISR vertical drifts [Chau and Woodman, 2004]. Vertical is perpendicular north at the magnetic equator where the B field is horizontally directed from the south to the north. The zonal ion Doppler velocities from the east-west JULIA beam are in reasonable agreement with the ISR zonal ion velocities. Although 150-km echoes have been observed and studied for many years, the physical mechanism which causes them is still unknown. This JULIA database of representative zonal and vertical (perpendicular north) ion drifts could contribute in providing very precise proxy measurements of F region drifts using less powerful and more economical radar.Kauai, Hawaii MF RADARThe Kauai, Hawaii (22.0N, 159.3W; 2 m alt) 1.98 MHz MF radar has been in operation since 1990. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (22.6, -91.5) degrees. The magnetic inclination and declination angles were 38.6 deg and 10.1 deg. The magnetic local time at 0 Universal Time (UT) is about 1249 MLT. The solar local time (SLT) is UT minus 10 hours and 37 minutes (-159.3/15.=-10.620).1270KAUhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltrTirunveli India MF radarTIRhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:tirThe Tirunelveli, India (8.67N, 77.82E; 30 m alt) 1.98 MHz MF radar has been in continuous operation since December 1992. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (6.8, 149.8) degrees. The magnetic inclination and declination angles were 1.4 deg and -2.6 deg. The magnetic local time at 0 Universal Time (UT) is about 0554 MLT. The solar local time (SLT) is UT plus 5 hours and 11 minutes (77.82/15.=5.188).
The original data files are hourly averages of the zonal and meridional velocity in Indian Standard Time (IST), which is 5 hours and 30 minutes later than UT. Samples are taken every 2 min, so a possible 30 samples can be had between IST 0:00:00 and IST 0:59:00, which is labelled as hour 1:00:00 IST. These times have been converted to the mid-point solar local time (or 0:11 SLT or 0.188 SLT for this example).
The MF radar system is identical to the one operating at Christmas island (2E,158W) and designed by Robert Vincent (robert.vincent@adelaide.edu.au) of the University of Adelaide in Australia (Vincent, 1991). The operating frequency is 1.98 MHz, with a peak transmitter power of 25 kW. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 millisec during the day and 25 millisec during the night. There are 32 coherent integrations during the day and 16 at night, using 256 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, want about 2 min or 102.4 sec integration during day and night, or 12.5x10-3sec * 32 integ * 256 samples = 102.4 sec and 25x10-3sec * 16 integ * 256 samples = 102.4 sec.]
The height coverage is 68-98 km during the day and 70-98 km during the night. The pulse width is 30 microsec, giving a height resolution of 4.5 km assuming a simple rectangular wave pulse [range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 30x10-6s / 2 = 4.5 km]. However, neutral velocities are given every 2 km between 80 and 98 km since the ionization is less below 80 km. 1254The Rarotonga, Cook Islands (21.21S, 159.77W; 2 m alt) 1.98 MHz MF radar has been in operation since 2000. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (-22.9, -84.9) degrees. The magnetic inclination and declination angles were -39.5 deg and 13.5 deg. The magnetic local time at 0 Universal Time (UT) is about 1316 MLT. The solar local time (SLT) is UT minus 10 hours and 39 minutes (-159.77/15.=-10.651).Rarotonga Cook Islands MF RADAR1245RTGhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltrThe EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981.
The power profiles are calibrated with an on-site ionosonde, and are then corrected for Te and Ti effects which are deduced from the auto-correlation functions (ACFs). The collision frequency model used is the CIRA 1972 model atmosphere in Banks and Kockarts (1973), in Aeronmy Part A. The NO+ composition is assumed zero above 300 km. Perpendicular and parallel ion velocities were calculated routinely beginning in March, 1990.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eisEISCAT I.S. Radar70EIS70The Syowa South HF radar is located in Antarctica (69.00 S, 39.58 E) and looks over a section of ionosphere poleward (southward) of 70 deg S that includes central Antarctica. It has operated since 1995. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Syowa velocity data is located at SANAE (South African National Antarctic Expedition), Antarctica.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 159 deg E of N, or about 52 degrees west of the general scan position of Syowa East. SYF830http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:syfSyowa Antarctica HF RadarISThttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:istThese experiments are a compilation of Irkutsk ISR data available in October 2002 from http://62.76.21.18/cgi-bin/madrigal/madInvent.cgi This is the first contribution from the Irkutsk IS radar,
Geographic: 52.9N 103.3E 502m-msl
Magnetic: 41.06N 104.75E
which started full operation in 1996, although there are some single measurements from 1988.
These data (for 1999 to 2002) have 50km spatial resolution, typically starting at 250-300 km height and with time resolution 20 minutes. The data are in the vertical direction.
Higher resolution is available on request with as little as 10 km height intervals, starting at 170-200 km, and 2 minutes time resolution.
The data can be used under the 'Rules of the Road' - ie, informing us at an early stage of the work and offering us a cooperation request at the publication stage.Irkutsk Russia I.S. Radar535160Arecibo P.R. Fabry-PerotAFPhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:afpThe Arecibo Observatory Fabry-Perot interferometer (18.35N, 66.75W) has been in operation since 1972. The data reported here (1980-1988), are atomic oxygen measurements at 630.0 nm. According to the IGRF model, the magnetic declination angle at Arecibo varied between -9.4 and -10.4 degrees between February 1980 and July 1988, while the inclination angle varied between 48.8 and 47.9 degrees. All nights are clear, or had cloudy periods removed. The approximate emission height is assumed to be 300 km. Scans in azimuth were done at a 30 degree elevation height, with usually one zenith measurment per scan.
The intensities are relative, (Code 2505) but are approximately correct to within a factor of two of the true emission intensities in Rayleighs. The Doppler half-width is related to the square root of the neutral temperature assuming a Gaussian emission shape. The instrument was not optimized to measure Doppler widths, but was broadened to increase the signal throughput in order to make better measurements of the Doppler shift, which is related to the neutral velocity. Because of uncertainties in the half-width, the conversion to temperature was not made.
In some of the data files the zenith observations were used as a zero reference in the analysis (Code 4050=1), while for others, all of the measurements for a given night were used (Code 4050=0) by assuming that each component of the horizontal neutral wind velocity can be represented by a second order Taylor expansion (constant horizontal velocity gradients) about a point directly above the station. A harmonic analysis gives the zonal (Ue) and meridional (Un) velocities, and two parameters related to the deformation of the flow, d(Ue)/dx and d(Un)/dy, where x and y are the eastward and northward directions, respectively. The vertical wind velocity (Uz) is thus not measured directly, but is derived from the DC term of the expansion. Values of Uz are inferred as the product of the horizontal divergence of the horizontal wind velocity, Uh, and the neutral scale height H: i.e., Uz = H del(Uh) where H = 50 km.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dvsDavis Antarctica Spectrometer3010The Davis, Antarctica (68.48S, 77.97E; 25 m alt) Czerny-Turner (CZT) scanning spectrophotometer obtains mesosphere temperatures from ratios of the hydroxyl (OH) (6-2) band during nighttime hours. The spectrophotometer was in campaign operation March to October 1990 and April to August 1994, and has had continuous winter operations since March 1995. (See Greet et al., 1998; French et al., 2000; Burns et al., 2002.)
Hydroxyl (6-2) band rotational temperatures are derived using Langhoff et al. (1986) transition probabilities, which are approximately 2 K higher than the temperatures derived by French et al. (2000) using experimentally derived P1 branch ratios with a slit width of 100 microns. The hydroxyl layer is centered at a mean height of 87+/-4 km with a mean thickness of 8 km. WINDII data showed that the hydroxyl layer often (up to 25% of the the time) has 2 peaks between 83 and 93 km (She and Lowe, 1998). The brightness of this layer usually decreases during the night.
The spectrophotometer has a 6 degree field-of-view (fov) that was aligned 30-degrees above the horizon in a direction +130 E from Davis away from auroral precipitation in 1990 (Greet et al., 1998). An order separating filter was not used in 1990. Starting in 1994, the optical axis was aligned in the zenith, with a resultant area of about 8 km x 8 km at 87 km. In practice the field of view is defined by the diffraction grating. The diffraction grating rotates about the vertical axis as it scans, so that the area of the grating directly viewing the sky decreases with wavelength (when the grating is at vertical the fov is zero). Thus the fov corresponding to the grating vertical axis varies with grating rotation angle and consequently with wavelength. The instrument is aligned towards the SE (+130 E), but rotates about the vertical as the spectrum is sampled, so these observations are considered to be in the vertical. DVShttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:jroJROJicamarca: Paracas Peru antenna11SANAE Antarctica HF RadarThe SANAE (South African National Antarctic Expedition) HF radar is located in Antarctica (71.68 deg S, -2.85 deg E) and looks over a section of ionosphere poleward of 65 deg S that covers much of East Antarctica. It has operated since 1997. The facility is part of the SuperDARN network of HF radars that extends from Alaska to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of SANAE velocity data is located at Halley Station.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. It has no second array for deriving elevation angle information. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is usually 7 sec, and the scan repeat time is then 120 sec (2 min). Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 107.0 deg E of N. SANhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:san825http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cofCollm LF RadarThe Collm Geophysical Observatory (51.31 N 13.003 E) uses the closely spaced receiver method at 177, 225, and 270 kHz. Two receivers are used to the geographic north and east of the radar so the center of the reflection point triangle is near (52 N, 15 E). The measurements of the nighttime neutral winds and virtual heights are averaged over half-hour intervals from measurements of about 3/minute for winds and about 300/minute for virtual heights.
The virtual height of the half-hour means is converted to true height using an empirical relation with linear height reduction (Kurschner et al, 1987). Then the half-hour means of the zonal and meridional winds are put through a multiple regression analysis to determine the altitude dependance of the prevailing and semi-diurnal tidal winds. To improve the spectral sensitivity, it proved useful to assume a circularly polarized tidal wind, which is acceptable for mid-latitudes. Therefor, the amplitude of the zonal and meridional semi-diurnal tidal wind is equal, and the phase of the meridional wind is 3 hours earlier than that of the zonal wind. Similarly, the amplitude of the zonal and meridional diurnal tidal wind is equal, and the phase of the meridional wind is 6 hours earlier than that of the zonal wind. However, the 24 hour component is normally only computed for the height of 95 km where the signal is a maximum. The result should be treated with some caution considering the fact that the observations are nighttime only.
The phases are in mean local solar time (SLT). There is 1 hour between SLT and UT since the measurements are near 15E. Most of the calculations are for the period of a month. Extra information of interest such as seasonal transitions and the quasi two-day wave are in catalogue records. The data in the CEDAR Data Base are from January 1993 to January 1997, with selected Lower Thermosphere Coupling Study (LTCS) periods earlier. 1320COFThe Sondre Stromfjord Fabry Perot interferometer, operated by the Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences of the University of Michigan is located at latitude 66.99N and longitude 50.95W. The invariant latitude is 74 degrees, the inclination of the magnetic field is 80 degrees and the declination of the field is -39 degrees (39 degrees to the west). Midnight local solar time at the site occurs at 03:24 UT, while midnight magnetic local time is 01:57 UT at the equinoxes. Magnetic midnight varies with season, being 15 minutes earlier at the winter solstice and 15 minutes later at the summer solstice compared to the equinox value.
Currently, the interferometer observes the line profiles of the forbidden emissions OI (557.7nm) and OI (630.0nm). Most of the data in the CEDAR Database are 630.0nm (code 7001), with additional 557.7nm (code 7002) data starting in 2002. The filter wheel was changed in 2002, resulting in brighter relative emissions. 5480Sondre Stromfjord Fabry-Perothttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sfpSFPSPMhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:spmSouth Pole, Antarctica Michelson Inter.A near infrared (NIR) BOMEM MB160 Michelson interferometer (MI) has operated at South Pole Station (90.00S, 2835 m) in Antarctica since January 1992.
The MI scans the dark sky NIR airglow emissions between ~5000-10000 cm-1. A periscope directs the airglow into the MI sequentially from three locations at an elevation angle of 25 deg at azimuth angles of 0 (0 E), 120 (120 E), and 240 (240 E) deg. The periscope dwells at each position for about 4-15 min. Airglow hydroxyl Meinel (OH-M) band emissions peak at 87 km and are located between about 83 and 89 km for an elevation angle of 25 deg, the 87 km peak is located at a latitude spacing of 1.6 degrees, or at 88.4 S. 5700The Vostok ground magnetometer station is located in Antarctica (-78.463 S, 106.826 E) and has been operated by the Arctic and Antarctic Research Institute of St. Petersburg since 1958. The analog data have been digitized for 1978 and 1979, and for 1983-1995. A 1-sec digital magnetometer was installed in 1996. The station is part of the former Soviet Union's scientific exploration of Antarctica, which started in 1957 during the International Geophysical Year (IGY). It is located near the center of the Antarctic ice sheet, about 3488 m above mean sea level, and about 1250 km from McMurdo and about 1500 km from Mirny on the coast.
Vostok is located in the polar cap at a high magnetic latitude. In 1978, the magnetic field at the surface was about 60950 nT, with an inclination angle of -77.682 degrees, a declination angle of -11.835 degrees, and an apex magnetic location of (-83.30, 53.56). In 2001, the magnetic field at the surface was about 59470 nT, with an inclination angle of -76.807 degrees, a declination angle of -12.019 degrees, and an apex magnetic location of (-83.31, 55.11). The apex magetic location of -83.3 is very close to the corrected geomagnetic (cgm) location of -83.4 cgmlat used for Vostok. Polar Cap Geomagnetic Index: Vostokhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pcv220PCV835http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:kgfThe Kerguelen Island HF radar is located in the southern Indian Ocean (49.35 deg S, 70.28 deg E; 58.9 mag S) and looks poleward. It has operated since 2000. The facility is part of the SuperDARN network of HF radars that extends from Alaska to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of SANAE velocity data is located at Syowa-East station.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. It has no second array for deriving elevation angle information. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is usually 7 sec, and the scan repeat time is then 120 sec (2 min). Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 107.0 deg E of N. KGFKerguelen Is. HF radarA Fabry Perot Interferometer is operated by the British Antarctic Survey at Halley, Antarctica. The station is sited on a floating ice shelf that drifts westward at around 800 m per year, requiring a new station to be built further to the east about every 10 years or so. The geographic coordinates are 75.5 deg S, 26.6 deg W, and the invariant geomagnetic coordinates are 61.5 deg S, 28.9 deg E. The magnetic inclination is 64 deg and magnetic north is 2 deg west of geographic north. The mean local time is 1 hour and 46 minutes (-26.6/15.) before Universal Time. The station was closed in 1998.5020http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:hfpHFPHalley Antarctica Fabry-PerotArrival Heights Fabry-Perot Interf SpAHFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ahfThe Fabry-Perot Spectrometer at Arrival Heights, Antarctica (77.8296 S, 166.6627 E, 190.3 m ASL) has been operated since 2002 by the Department of Earth and Space Sciences, University of Washington. The apex magnetic coordinates of Arrival Heights at 250 km height in 2002 were (-80.1, -34.3) with a magnetic declination of 142.6 deg, an inclination of -81.3 deg, and 0 UT at 17.15 MLT.
The dispersing element of the spectrometer is an air-spaced, 14 cm diameter effective clear-aperture Fabry-Perot etalon, which is both self-aligning and self-stabilizing. It is operated near the optimum operational point (2.0 cm spacer) for kinetic temperature determinations (Hernandez, 1988).
The spectrometer operates simultaneously at two wavelengths, which are arbitrarily selected by the use of dichroic mirrors and narrow (0.3 nm wide) interference filters. The inherent stability of the spectrometer is about 0.5 m/s (632.8 nm) for periods of months, because of its self-stabilizing properties. The instrumental internal stability calibration is updated every 9 s.5015180http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eqbMidnight Equatorward BoundaryThe Defense Meteorological Satellite Program (DMSP) has launched DMSP satellites since the mid 1970s. All the satellites have had precipitating particle spectrometer sensors (SSJ2-J4) on board. The SSJ4 sensor was first flown on DMSP-F6 in late 1982, so 1983 is the start of the automatically computed equivalent boundary data set. The official name of the index is "The Air Force Research Laboratory Auroral Boundary Index" and should be acknowledged as being provided by the USAF Research Laboratory, Hanscom AFB, MA. A courtesy copy of any publications using the index should also be sent to Dr. M. Susan Gussenhoven-Shea or her replacement, Dr. Katharine Kadinsky-Cade, at Air Force Research Laboratory, VSBXS, 29 Randolph Road, Hanscom Air Force Base, MA 01731-3010.
For most of the DMSP orbits on a given day, the auroral oval is crossed twice in each hemisphere, once on the ascending leg, and once on the descending leg. The auroral oval expands during increased auroral or magnetic activity and the equtorward boundary is strongly related to Kp (Gussenhoven et al., 1981). The poleward boundary is more difficult to detect than the equatorward boundary, so only the equatorward boundary is found automatically. Hand selection of the equatorward boundary is described in Gussenhoven et al. [1981, 1983]. The magnetic latitude of the equatorward boundary of the aurora is found for a particular orbit at a particular MLT. Then the magnetic latitude of the equivalent equatorward boundary at midnight magnetic local time (0 MLT) can be estimated by statistically determining the position of the auroral oval for every local time sector as a function of some magnetic activity index, such as Kp.
A computer algorithm was written to select the boundaries imitating the rules for hand selection with a quality flag of: 'best', 'good', 'not good'. Only those flagged as 'best' are released. Determination of the quality depends on a variety of factors. Generally,the clearest boundaries occur premidnight, that is, on the evening side, but not prior to 17 MLT. The next best are on the dawn side. Here, however, the flux levels are decreasing and the boundaries are not sharp. The worst boundaries are on the dayside, and near midnight when the oval is cut obliquely. Therefore, the preponderance of boundaries with the 'best' flag are on the evening side. Only 1/3 of the total are 'best' boundaries.
The equivalent equatorward boundary determined for 0 MLT is always defined positive, regardless of the hemisphere of the satellite. These data are also available as yearly files from the contact persons. The ftp and web sites at AFRL have been disconnected. Publically available plots from 1983 are at /instruments/eqb.html.EQBhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:stsSaint Santin: Montpazier receiverSTS43The incoherent scatter transmitter station at St. Santin, France (44.6N, 2.2E) operated between 1963 and 1987. The CEDAR Data Base holds all the data taken from 1966 until the end. Up until June 1973 and after July of 1986, the only receiver station operating was located at Nancay (47.4N, 2.2E). Between 1973 and 1986, 2 other receivers also operated at Montpazier (44.7N, 0.8E) and at Mende (44.5N, 3.45E).
In general, the daytime height range is 105 to 350 km, while the nighttime height range is 200 to 500 km. Before January 1, 1969, the faraday correction is not taken into account in the computation. The spectrum are analysed following the scheme described in Waldteufel (1970). The ion drift component is quasi parallel to the magnetic field as measured by the Nancay receiving station. Because the transmitter is not located at the receiving location, the bisector velocity is plotted for the period when only Nancay data were received. When all 3 receivers were on, then the data are 30 minute averages and the ion drifts in the geomagnetic coordinate system are calculated.
There are 4 areas in the summary plots. There are image plots as a function of height and time of the electron density, electron temperature, and ion temperature. Bin sizes are 40 minutes in time and 40 km in height. For the Nancay period alone there is also an image plot of the bisector velocity, while this is replaced by line plots of the ion drift in the perpendicular east, north and parallel directions at the altitude closest to 300 km. when there are 3 receivers.43ARO20http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aroThe incoherent scatter radar at the National Astronomy and Ionosphere Center (NAIC) at Arecibo, Puerto Rico (18.3N, 66.75W), has made ionospheric measurements since 1963. The radar facilities are shared with radio astronomers.
The most recent analysis solves between 3 (Ne, Ti, Ti) and 5 parameters (Ne, Ti, Te, H+/Ne, He+/Ne) simultaneously. The line-of-sight velocity is found in a separate fit to the slope of the auto-correlation function (ACF). There are several corrections that are applied to the data. These include a chirp correction for the velocities, eliminating bad data records due to satellites or ground based radio communication (some outliers remain), and calibration of electron densities with ionosonde data in post processing.
In the lower altitudes, a molecular ion model is assumed. The model was determined by looking for consistency in the other parameters. The molecular ion mass is assumed to be 30 amu and the assumed molecular ion composition is:
Alt(km) 145 182 219 256 > 293.
[M. ion]/[Ne] 1. 0.3 0.2 0.07 0.
Arecibo P.R. I.S. RadarEIS72The EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981, and recently expanded to include a facility at Svalbard, which will have its own web page when data are included in the CEDAR Data Base.
EISCAT: Tromso antennahttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eis72310http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:gcmGCMNCAR TGCM/TIGCM Model OutputThe NCAR TIGCM models output neutral winds and temperature. Specific TIGCM results are shown for the storm of March 22, 1979. The other results are of generic runs with the TIGCM which are described in Fesen (1997, JASTP, 785).
The TIGCM model solves and saves 16 parameters: ht, Tn, un, vn, wn, N2, O2, O, N(4S), N(2D), NO, Te, Ti, Ne, O+, and O2+. The O+-O collision frequency was increased by a factor of 1.7 in the model over the laboratory value, as recommended by Burnside et al (1988, JGR, 8642) and Salah (1993, GRL, 1543).
The model has 36 latitudes between -87.5 and +87.5 degrees geographic every 5 degrees apart, 72 longitudes between -180 and +175 geographic every 5 degrees apart, and 25 pressure levels between 97.5 km and approximately 500 km.
This data set has interpolated (or extrapolated) values of the neutral zonal and meridional wind and neutral temperature at 22 heights between 100 and 500 km for all 36 latitudes at 24 longitudes every 15 degrees apart between -165 and +180 degrees. The diurnally reproducible results were saved for 25 UTs, and then harmonic analyses of these parameters were computed.
Eighteen generic runs were made in 1993 for solar minimum (1976, with an assumed solar flux (350) of 75) and solar maximum (1979 with an assumed solar flux of 195), for three seasons (days 80, 172, and 355), and for three levels of activity (5 GW + 30 kV, 11 GW + 60 kV, and 33 GW + 90 kV). The activity is based on the hemispheric power and the polar cap potential drop. The IMF By was assumed to be 0 nT in the parameterizations. The 1989 Forbes and Vial semidiurnal tides appropriate for March, June and December were put at the lower boundary (97 km). Another version of these runs was for 70W only.
The summary plots show the wind fields on the temperature over the globe at 300 and 140 km every 4 UT hours on March 22, 1979, and at 0 and 12 UT for the generic runs. Only the 60 kV case was plotted for the generic runs in solar minimum (sflux=75) and solar maximum (sflux=195) for March, June and December.
The tidal fields for the neutral temperature and neutral zonal and meridional wind are shown at 140 and 300 km for the generic runs as a function of longitude and latitude. The 4 plots show the mean and the 24, 12 and 8-hr tidal amplitudes. Only the 60 kV case was plotted for the generic runs in solar minimum (sflux=75) and solar maximum (sflux=195) for March, June and December. The Fesen (JASTP, 1997) reference shows the tidal variations also as a function of height and magnetic activity for 70W. The Incoherent Scatter routine measurement with the MU (Middle and Upper atmosphere) radar (34.8N, 136.1E) uses 4 beam directions simultaneously, with the first 15 minutes of each hour devoted to single-pulse measurements (for electron density), and the last 45 minutes devoted to two-pulse (for ion drift velocity) or four-pulse (for ion/electron temperature) measurements. The radar operates at a frequency of 46.5 MHz and uses a beam width of 3.7 degrees. Measurements have been taken about 2 days per month starting on September 17, 1986.
The 4 beams are at an elevation angle of 70 degrees pointing towards magnetic north, east, south and west, assuming a declination angle of -5 degrees. The inclination angle is about 48 degrees, and the corrected magneitc latitude of the MU radar is about 25 degrees.
The initial range resolution of the velocities is 38 km. Velocities are averaged between 220 and 455 km, where the altitude of the measurement is defined to be 338, the midpoint of the 235 km range. A running 3-hour average of the ACF is computed as well as the height average before the line of sight (los) ion drift velocity is computed, so there are no error bars. The UT time is the midpoint of the 45 minutes of the middle hour. MUIhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:muiMU I.S. Radar, Shigaraki Japan25Thule Greenland Fabry-PerotTFPThe Thule Fabry Perot interferometer, operated by the Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences of the University of Michigan is located at latitude 76.53N and longitude 68.44W.5540http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:tfp5190http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:khaKitt Pk H-alpha Fabry-PerotKHAThe Wisconsin H-alpha Mapper (WHAM) Fabry-Perot Interferometer is operated at the Kitt Peak National Observatory by the Wisconsin Galactic Astronomy Group with support from the National Science Foundation.
The Wisconsin H-alpha Mapper (WHAM) Fabry-Perot is located at the Kitt Peak Observatory (31.98N, 111.60W; alt 2120.0 m), and has been operated remotely by the University of Wisconsin Galactic Astronomy Group since 1997 [Reynolds, 1997; Haffner et al., 2003]. The geocoronal atomic hydrogen is studied using the H-alpha (656.274 nm) and H-beta (486.1 nm) emissions. The WHAM instrument is a double-etalon Fabry-Perot coupled to a Charge Coupled Device (CCD) camera where the optics are designed to image the Fabry-Perot annular interference pattern onto the CCD. Hence, the CCD images are spectral and not spatial. The geocoronal atomic hydrogen can be observed both at H-alpha (6563 A, ~1-10 Rayleighs), and H-beta (4861 A, ~0.25-1 R).
The terrestrial H-alpha emission is primarily excited by the line center portion of the solar Lyman-beta emission and thus depends on both the solar excitation flux and the density distribution of upper atmospheric hydrogen. To first order, the column of H-alpha emissions (code 2502) observed by the Fabry-Perot comes from the sunlit portion of the geocorona above the Earth's shadow. Since density falls off with height, the shadow height (code 186) is roughly just below the peak emission height. However, a portion of the signal (~1-2 R) is also due to multiple scattering of Lyman-beta radiation below the Earth's shadow height in darkness. This contribution becomes increasingly significant for observations at higher shadow altitudes. The solar zenith angle (code 180) for all observations is below the horizon (e.g. nighttime conditions).
The semi-raw spectral images are saved in FITS (.fts) format where only a portion of the chip was used and the read noise was reduced using 4 x 4 on-chip binning [Haffner et al., 2003]. The CEDAR Database FITS files include additional header information on the observing geometry, wavelength (H-alpha set at 6564 A in the original .fits headers starting in 2001), kinst (5190) and kindat (7001 for H-alpha or 7101 for H-beta).
The kindat 17000 series files contain information from the H-alpha spectral profile (.spe) where the annular interference pattern in the .fts file is summed. Equal area annuli correspond to equal spectral intervals (measured in wavenumber, so the arbitrary pixel intensities are summed in equal area annuli to produce a spectral profile of relative emission as a function of wavenumber expressed as spectral displacement in velocity units km/s with an arbitrary zero (code 2416). The relative emission is divided by the exposure time (code 60) from the .coors file to create a relative emission rate (codes 4145 for NAN calibration files and 4146 for other files). Hot pixels due to cosmic rays, dark counts, reflections and a constant average bias have been removed. The standard deviation of the relative pixel intensity in each annuli divided by the exposure time is reported as the 'error bar' for the data point (codes -4145 and -4146). Codes 2507 and 2509 are the relative annular emission after the data have been normalized with a white light flat field (from the .dat files) divided by the exposure time to make an emission rate. The initial 31 spectral displacement points (below the arbitrary value of -50 km/s) are outside the aperture and are removed in the original .dat file and also in kindats 17000-3,17100-3.
Additional information in nightly catalog files come from the headers from the FITS files and from shadow altitude calculations. This information is listed in the nightly .shad and .coors files. The UT times in the names (codes 4142 and 4143) of the original FITS files (.fts) are from .log file UTs that are contained in companion nightly catalog files. The actual UT start times listed in the FITS headers are a few seconds later than the UT start times in the .log file and reflect when the commands were started by the WHAM instrument.
Astronomical locations are given in two coordinate systems: (1) galactic coordinates with galactic longitude b in degrees (code 193) and galactic latitude l in degrees (code 195), and (2) equatorial coordinates with right ascension (RA) in hours (code 192) and declination in degrees (code 194).
The hour angle (code 191) is defined as the difference between the Local Siderial Time and the Right Ascension of the object. The hour angle is zero when the target transits the Local Meridian, which passes through the zenith direction. Hour angles are negative when the object is rising, and are positive when the object is setting. Atmospheric extinction is minimized when zenith angles are restricted to 50 degrees or less (ZA<50), which are equivalent to elevation angles (code 142) of 40 degrees or more (el>40).
Typically, WHAM locks onto a given astronomical location for integration times (code 60) of 30 to 600 seconds, so the azimuth and elevation angles (codes 132 and 142) are initial values, while RA and DEC (codes 192 and 194) remain constant.
All observations of H-alpha column emissions from the thermosphere plus exosphere are made at night during moonless conditions. All observations reported to the CEDAR Database are also made during clear sky conditions, since even high cirrus clouds can affect the H-alpha signal. Acceptable values of the quality code 4144 are:
1. =A Excellent conditions
2. =A- Clouds sighted much later or earlier in the night
3. =B Clouds sighted within a few hours of the observation OR spectrum close to sunset or sunrise at the observatory OR ZA>50 (el<40)
-32767 Missing (consider ZA<50 or el>40 as best data)
If the wing of a spectrum is truncated, then its grade is reduced. Sometimes a grade is given for each spectrum, sometimes for a single night, and sometimes grades are missing (-32767). Single nightly grades show as text in the nightly catalog record, and are marked as missing for each spectrum without an individual grade. Spectra with ZA>50 (el<40) are of lower quality. For ZA>80 (el<10), the data can be so compromised (e.g. very low emissions rates) that they were not included in this database.
The regions of low galactic emission are useful for geocoronal observations because uncertainty in the retrieval of the geocoronal emission due to the presence of galactic emission is minimized. The fitting does not require removing the galactic emission in the low galactic region of observations. Geocoronal observations are also available from zenith and other directions, especially in survey runs. The analysis for survey data may include one or two Gaussians in the fit, while the cleaner low galactic emission regions are usually analyzed using two Gaussians to account for fine structure. The absolute intensities (code 2502) are calibrated using the bright H-alpha emission at (RA 20.97, DEC 44.6 or l,b 85.60 -0.72) of 800 R +/-10% from the North American Nebula (NAN). There is an additional ~5% uncertainty in the relative calibration due to night-to-night variability in the transmittance of the atmosphere. These uncertainties are larger than the standard deviation (codes -4145 and -4146) of pixel intensity in the annuli divided by the exposure time.
Locations (code 4141) used for geocoronal observations or calibrations combined with the H-alpha kindats are:
* -1/17001 = NAN (North Amercian Nebula calibration source)
* 0/17000 = zenith (geoz, useful to compare with some models)
* 1/17003 = surveys or other at all different (non-zenith) directions
* 7/17002 = Lockman (low galactic emission region at l,b 148.5 53)
* 8/17002 = Newoff (low galactic emission region at l,b 163.5 53.5)
* 9/17002 = HD93521 (low galactic emission region at l,b 183.14 62.15)
* 10/17002 = Off01 (low galactic emission region at l,b 166.7 26.31)
* 11/17002 = Off02 (low galactic emission region at l,b 140.97 50.07)
Further details of the procedure are in the references, in the generic kindat catalog records, and are available from the contact persons.Scott Base Antarctica MF RadarSBFThe Scott Base MF radar (78 S, 167 E) in Antarctica is operated by the Physics Department of the University of Canterbury, Christchurch, New Zealand. It uses the partial-reflection, spaced antenna method (Fraser, 1984b) and has contributed to mean wind and tidal studies (Avery et al, 1989; Fraser 1984a, 1989; Fraser et al 1989; Manson et al., 1989, 1990, 1991). The mean solar local time (SLT) is about 11 hours and 8 minutes ahead of Universal Time (UT) (i.e., 167 E / 15 deg/hr = 11.13 hours = 11 hrs 8 min). The phases are in SLT.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sbf1210FPFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:fpf5240Fritz Peak CO Fabry-Perot Interf SpThe dispersing elements of the spectrometers are air-spaced, 14 cm diameter effective clear-aperture Fabry-Perot interferometers, which are self-aligning and self-stabilizing (Hernandez and Mills, 1973). The instruments were operated at the optimum point for kinetic temperature determinations (Hernandez, 1979; 1988).
The spectrometers operated with narrow (<0.3 nm wide) interference filters -a necessity, in particular, for the 630.0 nm emission, in order to avoid contamination from the nearby OH emission lines (Hernandez, 1974). The inherent stability of the spectrometers is about 0.5 m/s (632.8 nm) for periods of months, because of their self-stabilizing properties. The instrumental internal stability calibration is updated every 9 s throughout the day, year round.
The spectrometer observed wavelengths with these Fritz Peak instruments have been the so-called red line (630.0 nm, kindat=17001, 1973-1985) and green line (557.7 nm, kindat=17002, 1969-1985) of atomic oxygen (OI) with typical emission height peaks in the range 210 to 300 km and 94-98 km, respectively. Each spectrometer observed a different wavelength.
The spectrometers observed the night-sky at the 4 cardinal directions at 20-degree elevation above the horizon, as well as zenith. Since the instruments are light-limited, the time spent in observing this 5-direction cycle can be as short as 5 minutes during auroral activity. The instrument is internally time-limited to spend no less that one-minute and no more than 15 minutes in any given direction. Other observing protocols, such as two orthogonal directions and zenith, have also been used. The observations were made every evening and only those with clear weather -as reported by an observer on site- are reported here. Because of the narrow filters used, operation of the instrument is not affected by moonlight. Typically, about 30% of the nights observed were clear.The College, Alaska Fabry-Perot interferometer was located on the roof of the Geophysical Institute in the years reported here (1981-1983). This is at 64.7N and 148.1W in geographic coordinates, where the corrected geomagnetic coordinates are 64.9N and 100.3W. This is relatively close to the Chatanika incoherent scatter radar site at 65.1N and 147.4W, which operated between 1971 and 1982. The IGRF model gives a magnetic declination angle of about 25 degrees and inclination angle of 76 degrees for the measurement period. However, the measurements were made relative to the magnetic field direction where the declination was assumed to be 30 degrees. This is not significantly different from the true declination, so the derived horizontal results are reported as being in the magnetic directions. The measurements are all at 630.0 nm. All nights included are clear, or had cloudy periods removed.
The zenith measurements are assumed to be on average zero throughout the night. All other measurements were taken in directions relative to the magnetic E, N, W and S directions at elevations angles between 20 and 45 degrees, and were converted to horizontal directions assuming an emission layer centered at 225 km.
The intensities are relative, (Code 2505) but are approximately within 25% of the true intensities in Rayleighs.5460CFPhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cfpCollege Fabry-PerotWUP3320The Wuppertal, Germany (51.3N, 7.2E) Czerny-Turner grating spectrometer scans in the near infrared between 1.05 - 1.74 um with a spectral resolution of about 450. It has been operated by the University of Wuppertal since 1980. The instrument measures the nightglow hydroxyl [OH*]. The [OH*] emission layer is centered near 87 km (+/-2 km) with a thickness of about 9 km.
Measured parameters are the hydroxyl Meinel band rotational temperature (Code 812) in tenths of Kelvin. To reduce NLTE effects as much as possible, the (3,1) transition lines P1(2), P1(3) and P1(4) near 1.5 um are chosen for the measurements. More than 3100 average nightly mean temperatures are available continously from July 1980 until now with a gap in 1985/86. The instrument field-of-view in the zenith has a horizontal resolution of 20x20 km^2 (with respect to 86 km altitude). One spectrum is measured in 90 s.
Rotational temperatures are derived from the relative intensities of the three lines. Hence, if there should be changes of spectrometer sensitivity, atmospheric transmission, or other factors the derived temperatures would not be affected unless such changes are wavelength dependent. Even in that case, influences would be small because the three line are close together (1.524 um, 1.533 um, 1.543 um).
The relative error of nightly mean temperature values is estimated to be 1-2 K. This is derived from measurements during the whole night, and therefore, it still contains some atmospheric variability. Thus, the value must be considered as an upper limit for the relative error. The absolute temperature error is of the same magnitude. Spectral and absolute intensity calibrations are performed about once per year.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:wupWuppertal Germany OH SpectrometerCIAThe Christmas Island ST (MEDAC) radar is located at (1.95N, 157.30W). The MEDAC (Meteor Echo Detection And Collection) sytem added to the ST (STratospheric) radar makes observations of winds measured from the backscatter off meteor trails. The system is described in Avery et al. (1990). The observations are described in solar local time, which is defined to be 10 hours and 32 minutes after UT (-158/15 = -10.53 or 10 hours and 32 minutes, where the longitude used was 158 W instead of 157.30 W). These are monthly means corresponding to the day numbers given. The days are counted from Hawaiian Standard Time (= UT-10h). Hence, data starting on the first of the month actually starts at 10 UT on the first of the month, and data ending at the end of the month ends on the first day of the next month at 0959 UT. This data set is two years of data from September 1988 to August 1989, and for all of 1991. The analysis will be revised in the future.2090http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ciaChristmas Island ST (MEDAC) RadarThe Syowa East HF radar is located in Antarctica (69.00 deg S, 39.58 deg E) and looks over a section of ionosphere poleward of 70 deg S that includes the east Antarctica ice cap and the southern ocean. It has operated since 1997. The facility is part of the SuperDARN network of HF radars that extends from Alaska to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Syowa velocity data is located at Kerguelen.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is usually 7 sec, and the scan repeat time is then 120 sec (2 min). Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 107.0 deg E of N, or about 52 degrees east of the look direction for Syowa South. Syowa East (Antarctica) HF Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:syeSYE831STMThe Stockholm, Sweden (59.5N, 18.2E) IR Michelson Interferometer (IRMI) scans in the near infrared between wavenumbers 6000 to 10,000 cm-1 (or in the range of 1000-1667 nm in wavelength), with a 4 cm-1 resolution (or 0.1% resolution, about 0.3 nm). The instrument is operated by Utah State University with support from Stockholm University.
The instrument measures the nightglow hydroxyl [OH]. The [OH] emission layer is centered near 87 km with a thickness of about 8 km. The center of the layer can vary between about 86 and 89 km, giving an error bar in the altitude of about +/6 km considering the thickness also. The rotational temperatures reflect the neutral temperatures in this altitude region. The measured parameters are the hydroxyl Meinel band rotational temperature in Kelvin and the hydroxyl Meinel integrated band radiance in kR and in log10(R).5860Stockholm Sweden IR Michelson Interfer.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:stm5465http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pkfPoker Flat AK Scanning Imaging F-P SpecPKFThe all-sky scanning imaging Fabry-Perot Spectrometer (ASIFPS) at Poker Flat, Alaska (65.12N, 147.43W) is also known as a Scanning Doppler Instrument (SDI). It is an extremely high resolution optical imaging spectrometer. It measures the angular distribution of Doppler shifts and of Doppler broadening of optical airglow and auroral light emitted from the Earth's upper atmosphere, across the entire sky scene that is visible to the gorund-based instrument, down to a zenith angle of ~75 deg. The distributions of Doppler shifts and of Doppler broadening across the sky are used to infer geographic maps of the wind and temperature distributions prevailing within the emission layer.
The instrument is located on a ridge-top, 50 km ENE from Fairbanks and at 440 m above mean sea level. It has been operated since November 1994 by the Geophysical Institute of the University of Alaska as part of the optical diagnostic instruments at the Poker Flat Research Range. The building is aligned in the magnetic north direction at 28.5 degrees azimuth to NE. The apex magnetic coordinates of Poker Flat in December 2001 at 240 km were (65.25, -95.41), with a magnetic declination of 23.56 deg to NE, an inclination of 77.36 deg to SW, and 0 UT at 1231 MLT. At 96 km, apex coordinates are (65.23, -95.45), with a magnetic declination of 24.28 deg, an inclination of 77.37 deg, and 0 UT at 1231 MLT. The observations are reported in approximate local magnetic coordinates, rotated 28.5 degrees clockwise from geographic, and also in geographic coordinates. The magnetic skew angle (code 1020) is about 4.6 deg, which is negligible.
The instrument is based on a 100-mm aperture capacitance-stabilized Fabry-Perot etalon, the plates of which are piezoelectrically scannable in spacing over approximately 1.5 orders of interference (at 630-nm) about a nominal 20-mm gap. Skylight is coupled into the etalon through an all-sky lens and optical relay system which maps an approximately 75-degree half-angle field-of-view onto 6 orders of interference at the etalon. Interference fringes formed by the etalon are conjugate with the sky. The sky, modulated by this fringe pattern, is re-imaged onto an intensified CCD detector, after first passing through a narrow-band interference filter. WHF910http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:whfStokkseyri (Iceland West) HF RadarThe Stokkseyri HF radar is located in western Iceland (63.86 deg N, -22.02 deg E) and looks to the west over a section of ionosphere that includes southern Greenland and northeastern Canada. It has operated since 1994. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Stokkseyri velocity data is located at Goose Bay in Canada.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provides the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is westward approximately 50 deg wide and is centered on -59 deg E of N. 1539Ascension Island Meteor RADARThe Ascension Island (7.96 S, 14.38 W; alt 170 m) 43.50 MHz meteor radar has been in operation since August 1999. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (-19.6, 55.0) degrees. The magnetic inclination and declination angles were -39.3 deg and -16.8 deg. The magnetic local time at 0 Universal Time (UT) is about 2235 MLT. The solar local time (SLT) is UT minus 58 minutes (14.38/15=0.959).http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltrASCThe incoherent scatter transmitter station at Kangerlussuaq (Sondrestrom), Greenland (66.99N, 50.95W, 185m ASL) has been in operation since February, 1983. It was moved from Chatanika, Alaska in 1982-1983, where it operated from July 1971 to March 1982. On day 359 of 2001 at 110 km altitude, the apex magnetic coordinates were (73.0, 40.5) degrees. The magnetic inclination and declination angles were 80.1 deg and -35.2 deg. The magnetic local time at 0000 Universal Time (UT) is about 2137 MLT. The solar local time (SLT) is UT minus 3 hours and 24 minutes (-50.95/15.=-3.397).SON80Sondrestrom I.S. Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sonhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:imfInterplanetary Mag Fld and Solar Wind120The CEDAR Database contains hourly Interplanetary Magnetic Field (IMF) and solar plasma data from various satellites from 27 November 1963 to 19 December 1999. One minute IMF data for World Day campaign periods are available from 13 April 1983 to 19 January 1988. Some data sources are:
* hourly IMF and plasma data (1963-present) at the National Space Science Data Center
* 2 min IMP MIT plasma data (1973-present) at MIT
* ISTP key parameters of IMF and solar plasma data from Wind (11/94-present), IMP-8 (10/73-present) and ACE (8/97-present) from http://nssdc.gsfc.nasa.gov/space/ndads/spycat.html
* Definitive WIND magnetometer (PI R. Lepping) 3-sec, 1-min, 1-hour data from Nov 1994-Jul 1999. In ascii at ftp site ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/wind/mag. Will also be available via CDAWeb.
* Last 3 months of IMF and solar plasma data from WIND and (IMF from MFI and plasma data from SWE) and near real-time data
* Last 3 months and real-time IMF and solar plasma data from ACE (IMF from MAG and plasma data from SWEPAM) at ACE lists. IMFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:rbmA near infrared (NIR) BOMEM MB160 Michelson interferometer (MI) has operated at Resolute Bay (74.68 N, 94.90 W), 1 m above mean sea level in Canada since September, 1996.
The MI scans the dark sky NIR airglow emissions between ~5000-10000 cm-1. The airglow is observed at an elevation angle of 25 deg towards the north (0 deg azimuth) and is averaged over about 6 min. Airglow hydroxyl Meinel (OH-M) band emissions peak at 87 km and are located between about 83 and 89 km. For an elevation angle of 25 deg, the 87 km peak is located at a latitude spacing of 1.61 degrees, or at 76.29 N, or 179 km away. 5950RBMResolute Bay, Canada Michelson Interf.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sts42STS42Saint Santin: Mende receiverThe incoherent scatter transmitter station at St. Santin, France (44.6N, 2.2E) operated between 1963 and 1987. The CEDAR Data Base holds all the data taken from 1966 until the end. Up until June 1973 and after July of 1986, the only receiver station operating was located at Nancay (47.4N, 2.2E). Between 1973 and 1986, 2 other receivers also operated at Montpazier (44.7N, 0.8E) and at Mende (44.5N, 3.45E).
In general, the daytime height range is 105 to 350 km, while the nighttime height range is 200 to 500 km. Before January 1, 1969, the faraday correction is not taken into account in the computation. The spectrum are analysed following the scheme described in Waldteufel (1970). The ion drift component is quasi parallel to the magnetic field as measured by the Nancay receiving station. Because the transmitter is not located at the receiving location, the bisector velocity is plotted for the period when only Nancay data were received. When all 3 receivers were on, then the data are 30 minute averages and the ion drifts in the geomagnetic coordinate system are calculated.
There are 4 areas in the summary plots. There are image plots as a function of height and time of the electron density, electron temperature, and ion temperature. Bin sizes are 40 minutes in time and 40 km in height. For the Nancay period alone there is also an image plot of the bisector velocity, while this is replaced by line plots of the ion drift in the perpendicular east, north and parallel directions at the altitude closest to 300 km. when there are 3 receivers.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:maf1220Mawson Antarctica MF RadarThese are tidal analyses of the mean neutral winds between 78 and 108 km over consecutive periods of 12 days between June 1984 and November 1990 from the MF radar located at Mawson, Antarctica (67.62 S, 62.89 E). The radar employs the "spaced antenna" method. The tidal analysis is a least squares fit at each altitude for the mean, diurnal and semi-diurnal components. The error is the standard deviation. Observations are made relative to mean solar time (SLT), which is about 4 hours and 12 minutes ahead of UT. (69.89 / 15 deg/hr = 4.19 hrs = 4 hrs 12 min). The diurnal and semi-diurnal tidal components are available for this data set, and can be obtained from R. Vincent. They will be submitted to the CEDAR Data Base in the future. Plots of the mean winds are available in Vincent (1993).
The integration time for these data is 12 days, which means that there is an overlap of days at the end of each year, and sometimes also just before the year's end. Echoes on the 12 days were binned into 24 1-hour bins of SLT. If only 15 hours or less of the full 24 hours were filled, then the tidal analysis was not performed. With 16-24 hours available, a least squares fit was made, where the values were weighted by the number of points and variance in each SLT bin. One should be wary of the results of analyses that are based on less than 20 hours of an SLT day.MAFThe Peach Mountain (also known as Stinchfield Woods) Fabry-Perot interferometer, operated by the Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences of the University of Michigan is located at latitude 42.40N and longitude 86.93W, and at an altitude of 955 ft.
Currently, the interferometer observes the line profile of the forbidden emission OI (5577 A) and OH (8920 A). The geophysical parameters obtained from the data reduction are the gas kinetic temperature of the emitting region from the natural width of the sky profile, the line of sight wind from the Doppler shift of the sky profile, and the surface brightness of the emission line. OI (5577 A) nightglow emission is generally believed to issue from the altitude range 85 to 300 km, with the major contribution originating from a narrow height interval roughly 10 to 15 km broad centered at 97 km. Similarly, the Meinel OH emission also issues from a broad altitudinal range though centered at a lower altitude. Thus, it is difficult to assign a unique altitude to each ground based OI (5577 A) and OH (8920 A) interferometer measurement. If no other information is available, we generally ascribe 97 km as the altitude of OI (5577 A) emission and 86 km for the OH emission.
Line of sight winds derived from the observed shift of the emission line from a zero reference position requires the determination of a zero wind. The reference zero wind is taken to be the average of an entire nights vertical wind data. Generally, the four cardinal directions are also sampled as well as the vertical. There is no exclusion of any data in the CEDAR Data Base, so cloudy night fits are also included. The cloud cover (code 440) measured by the Detroit Metro airport meteorological station is given in octas of the sky covered. Values range from 0 (clear) to 9 (overcast). In the summary plots, wind measurements were not plotted unless the cloud cover was 0-3. Temperatures and relative emission measurements were not plotted unless the cloud cover was 0-6.5300PFPhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pfpPeach Mountain Fabry-PerotEHFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ehf911The Pykkvibaer HF radar is located in western Iceland (63.77 deg N, -20.54 deg E) and looks to the east over a section of ionosphere that includes the Greenland sea and Svaalbard. It has operated since 1995. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Pykkvibaer velocity data is located at Hankasalmi, Finland.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provides the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is eastward approximately 50 deg wide and is centered on 30 deg E of N. Pykkvibaer (Iceland East) HF Radar221PCTPolar Cap Geometric Index: Thulehttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pcvDUMThese are monthly climatology neutral tidal winds in the mesosphere and lower thermosphere for data taken between 1978 and 1982 by the meteor wind radar at Durham, New Hampshire.
The meteor wind radar at Durham, New Hampshire (43.12 Deg.N, 70.94 Deg.W) has operated routinely during most years since 1974. The radar looks at 45 deg. elevation in the Northeast and Northwest directions with beamwidths of +-20 degrees. The system is a computer controlled coherent pulsed radar at 36.8 Mhz. Measurements are made of the direction cosines, slant range, and slant range doppler. Since a horizontal wind is assumed, only measurements with zenith angles less than 60 degrees are used in the tidal analysis. The height of the meteor trail reflection points have a Gaussian distribution centered at approximately 95 km with a standard deviation of approximately 9 km.
Significant results are achieved by averaging over 4 days. These are the 12 monthly climatologies created by binning 4-day averages over 5 years in the appropriate month. The tidal analysis is based on the method developed by Groves (1959) using 30 coefficients. The results are least mean square fits to the data. The error bars are about 8 m/s at 80 and 107 km, and are about 5 m/s at 95 km. The phases are given only to the nearest hour, which refers to Eastern Standard Time (EST = UT - 5 hrs). The local mean solar time for Durham is the Universal Time minus 4 hours and 44 minutes. 1620http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dumDurham N Hampshire Meteor Wind RadarThe Adelaide, Australia (34.56S, 138.48E; ~19 m alt) 1.98 MHz MF radar has been in operation since 1983 at the location of Buckingham Park, just outside of Adelaide. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (28.2,-149.8) degrees. The magnetic inclination and declination angles were 48.0 deg and -6.4 deg. The magnetic local time at 0 Universal Time (UT) is about 0856 MLT. The solar local time (SLT) is UT plus 9 hours and 14 minutes (138.48/15.=9.232). Code 42 (LST-UT) was corrected from 1.E-03 hr to hhmm in Sep 2004.
The original data files are hourly averages of the zonal and meridional velocity in Australian Central Standard Time (ACST), which is 9 hr 30 min later than UT. Samples are taken every 2 min, so a possible 30 samples can be had between ACST 9:00:00 and ACST 9:59:00, which is labelled as hour 9:00:00 ACST. The midpoint is 9:30:00 ACST or 0:00:00 UT, or 9:14:00 SLT. Local times have been converted to the mid-point SLT, or 14 min (0.232 hr) are added to the begin LT.
The MF operating frequency is 1.98 MHz, with a peak transmitter power of 25 kW, 50 kW starting in 1995. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 and 25 millisec, respectively during the day and night. There are usually 32 coherent integrations during the day and 16 at night, using 256 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, want about 2 min or 102.4 sec integration day or night, or 12.5x10-3sec * 32 integ * 256 samples = 102.4 sec and 25x10-3sec * 16 integ * 256 samples = 102.4 sec.]
The height coverage is 50-98 km during the day and 70-98 km during the night, at Adelaide. The pulse width is 30 microsec, giving a height resolution of 4.5 km assuming a simple rectangular wave pulse [range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 30x10-6s / 2 = 4.5 km]. However, the height range provided is every 2 km between 60 and 98 km. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:adf1240Adelaide Australia MF RadarADFPFRPoker Flat AK I.S. Radarhttp://cedarweb.hao.ucar.eduPoker Flat AK I.S. Radar61Christchurch New Zealand MF Radar1230CCFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ccfThe Christchurch MF radar (43.83 S, 172.68 E) in New Zealand is operated by the Physics Department of the University of Canterbury, Christchurch, New Zealand. It uses the partial-reflection, spaced antenna method (Fraser, 1984) and has contributed to mean wind and tidal studies (Fraser, 1968; Fraser 1989; Fraser et al 1989; Manson et al., 1989, 1990, 1991). The mean solar local time (SLT) is about 11 hours and 31 minutes ahead of Universal Time (UT) (i.e., 172.68 E / 15 deg/hr = 11.51 hours = 11 hrs 31 min). The phases are in SLT.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:uslUSU ALO Rayleigh LIDARUSL6330The Utah State University (USU) Rayleigh lidar at the Atmospheric Lidar Observatory (ALO) is run by the Center for Atmospheric and Space Sciences (CASS). It is located at Logan, Utah at (41.74N, 111.81W) on the roof of the Science and Engineering Research (SER) building on campus. The height is 1466 m using the WGS84 geoid to represent the earth. The lidar is operated in the vertical direction and can obtain data on all non-heavy cloud nights. (Thin cirrus clouds are OK.) An operator is present to operate the system and for aircraft safety. The lidar started operations in August 1993, with relatively regular operations up to the present except between April 1997 and May 1998 when the lidar was not operating.
The lidar operates at a wavelength of 532 nm up to about 500 km, but collects meaningful data only between about 45 and 100 km. The height resolution of the data is originally 37.5 m using 3600 shots (30 per sec) over 2 minutes. However, averaging is done over 81 range gates (81*37.5m = 3.0375 km) with a sliding average reported every 112.5 m (3 range gates). The number of 2-min integrations is reported as Code 415. Hourly averages of 29 or less 2 minute intervals are calculated, where cloudy or otherwise unusable periods have been eliminated in the hourly average (kindat=17002). Nightly average profiles are also computed.1390The Tromso MF radar is located in Norway (70 N, 19 E). The mean solar local time (SLT) is Universal Time (UT) plus 1 hour and 18 minutes. (SLT = UT + 1:18). The phases are in SLT and the measurement days start at 0 UT. The Tromso MF radar data is obtained and analyzed by the Saskatoon MF radar scientists, and has provided considerable mean winds (Manson et al., 1990a and 1991a) and tidal data (Manson et al, 1989). LTCS-1 and LTCS-2 are described for all middle atmosphere radars in Manson et al. (1990b, 1991b). MF radars use the spaced antenna method. Harmonic analysis is applied to hourly mean winds (weighted by data yield per hour) at individual heights to obtain tides for the prime LTCS or stated intervals. Typical standard deviations for means, 12-hour and 24-hour tides are in the above LTCS papers. Tides of the month for Tromso are means of 4-day fits (the amplitudes are arithmetic means). Data up to 99 km are real heights --- above, they are from the E-region, a layer about 5 km centered near 102 km.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:trfTRFTromso Norway MF Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mlhThe incoherent scatter transmitter station at Millstone Hill, Massachusetts (42.6N, 71.5W) has been in operation since 1960. The facility is part of and operated by the Massachusetts Institute of Technology.
ISR data comes from the fixed zenith antenna, the steerable antenna, or both.
The electron densities from the power profile were calibrated with an on-site ionosonde, where recently, this ionosonde has been the University of Massachusetts at Lowell digisonde. Since the Coast Guard uses some of the frequencies needed to properly scan the ionosphere, calibration can sometimes be difficult. The calibrated electron density is then corrected for Te and Ti effects, where Te and Ti come from auto-correlation fits. The calibration and auto-correlation fits now have the same height resolution, although in the past, the auto-correlation fits had lower height resolution.
The ion composition changes from mostly O2+ and NO+ at lower altitudes, to mostly O+, and then to H+ and some He+ at higher altitudes. Above 400 km, the percent H+ is computed along with the major ion O+. At lower altitudes, the ratio of molecular ions to the total number of ions is modeled as specified by the FORTRAN code segment below.
REAL FUNCTION PMF(Z)
Z1=AMIN1(-(Z-120.)/40.,50.)
H=10.-6.*EXP(Z1)
Z2=AMIN1(-(Z-180.)/H, 50.)
30Millstone Hill I.S. RadarMLH30YAMThe Yamagawa, Japan (31.20N, 130.62E; alt ~70 m) 1.9550 MHz MF radar has been in operation since 1994. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (25.1,-157.3) degrees. The magnetic inclination and declination angles were 44.7 deg and -5.6 deg. The magnetic local time at 0 Universal Time (UT) is about 0826 MLT. The solar local time (SLT) is UT plus 8 hours and 42 minutes (130.62/15.=8.708).
The original data files are 30 min averages of the zonal, meridional and 'vertical' velocity in UT. The UT time is the midpoint UT, and is also listed as the midpoint SLT. Samples are taken every 3, 4 or 5 min, so 6 to 10 samples can be had between UT 23:45:00 and UT 00:15:00. To improve data quality, 'median screening' is applied inside a 1-h bin. If data points lie outside a threshold standard deviation (code 4152) of usually 1.5 inside a 1-hr bin, they are discarded. So the low qulity (jamped) data are rejected and then the remaining data are averaged over 30-min bins with a threshold of usually 30% (code 4151). The number of points used in each direction are in codes 422, 423 and 424.
The 'vertical' velocities (code 1432, 'contaminated neutral vertical geographic wind (+up)') are from the beam in the vertical direction. The antenna array in a triangle has a different beam width for different azimuth direction, resulting in beam widths about 20-30 deg wide. Hence, the 'vertical' velocity will be contaminated by horizontal wind times the sine of 10 to 15 degrees (.17 to .26). Since the horizontal winds are stronger than the vertical winds, even the sign could be incorrect. The standard deviations of the 'vertical' winds are also larger than the average values.
The MF operating frequency is 1.95550 MHz, with a peak transmitter power of 50 kW. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 millisec during the day and 25 millisec during the night. There are 80 coherent integrations during the day and 40 at night, using 240 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, if want 240 sec or 4 min integration during day and night, then 12.5x10-3sec * 80 integ * 240 samples = 240 sec and 25x10-3sec * 40 integ * 240 samples = 240 sec.]
Data sampling is done every 2 km usually between 60-98 km for Yamagawa (60-108 km for Wakkanai, 44-108 km for Poker Flat). The height range of wind velocity data is variable accoding to atmospheric and radio conditions and is usually about 70-90 km at Yamagawa and Wakkanai during the day and 80-90 km at night (60-90 km/70-90 km for Poker Flat for day/night conditions).
The pulse width is 48 microsec (27 microsec before September 1996), giving a height resolution of approx. 7.2 km (4.1 km) assuming a simple rectangular wave pulse. For the 48-microsec case, the range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 48x10-6s / 2 = 7.2 km. However, neutral velocities are given every 2 km. Yamagawa Japan MF radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:yam1275WAKWakkanai Japan MF radarThe Wakkanai, Japan (45.36N, 141.81E; alt ~10 m) 1.9585 MHz MF radar has been in operation since 1996. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (38.9,-146.6) degrees. The magnetic inclination and declination angles were 59.8 deg and -9.6 deg. The magnetic local time at 0 Universal Time (UT) is about 0909 MLT. The solar local time (SLT) is UT plus 9 hours and 27 minutes (141.81/15.=9.454).
The original data files are 30 min averages of the zonal, meridional and 'vertical' velocity in UT. The UT time is the midpoint UT, and is also listed as the midpoint SLT. Samples are taken every 3, 4 or 5 min, so 6 to 10 samples can be had between UT 23:45:00 and UT 00:15:00. To improve data quality, 'median screening' is applied inside a 1-h bin. If data points lie outside a threshold standard deviation (code 4152) of usually 1.5 inside a 1-hr bin, they are discarded. So the low qulity (jamped) data are rejected and then the remaining data are averaged over 30-min bins with a threshold of usually 30% (code 4151). The number of points used in each direction are in codes 422, 423 and 424.
The 'vertical' velocities (code 1432, 'contaminated neutral vertical geographic wind (+up)') are from the beam in the vertical direction. The antenna array in a triangle has a different beam width for different azimuth direction, resulting in beam widths about 20-30 deg wide. Hence, the 'vertical' velocity will be contaminated by horizontal wind times the sine of 10 to 15 degrees (.17 to .26). Since the horizontal winds are stronger than the vertical winds, even the sign could be incorrect. The standard deviations of the 'vertical' winds are also larger than the average values.
The MF operating frequency is 1.95550 MHz, with a peak transmitter power of 50 kW. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 millisec during the day and 25 millisec during the night. There are 80 coherent integrations during the day and 40 at night, using 240 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, if want 240 sec or 4 min integration during day and night, then 12.5x10-3sec * 80 integ * 240 samples = 240 sec and 25x10-3sec * 40 integ * 240 samples = 240 sec.]
Data sampling is done every 2 km usually between 60-98 km for Yamagawa (60-108 km for Wakkanai, 44-108 km for Poker Flat). The height range of wind velocity data is variable accoding to atmospheric and radio conditions and is usually about 70-90 km at Yamagawa and Wakkanai during the day and 80-90 km at night (60-90 km/70-90 km for Poker Flat for day/night conditions).
The pulse width is 48 microsec (27 microsec before September 1996), giving a height resolution of approx. 7.2 km (4.1 km) assuming a simple rectangular wave pulse. For the 48-microsec case, the range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 48x10-6s / 2 = 7.2 km. However, neutral velocities are given every 2 km. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:wak1310EISCAT: Sodankyla antenna73http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eisThe EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981, and recently expanded to include a facility at Svalbard, which will have its own web page when data are included in the CEDAR Data Base.
EIS73EIS7171EISCAT: Kiruna antennahttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eisThe EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981, and recently expanded to include a facility at Svalbard, which will have its own web page when data are included in the CEDAR Data Base.
Kapuskasing HF RadarKHFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:khf845The Kapuskasing HF radar is located in northern Ontario (49.39 deg N, -82.32 deg E) and looks over a section of ionosphere poleward of 50 deg N that covers north-central Canada including Hudson Bay and the Canadian arctic archipelago. It has operated since 1993. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Kapuskasing velocity data is located at Saskatoon, Saskatchewan.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provides the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is westward approximately 50 deg wide and is centered on -12 deg E of N. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cslCSLColorado State Sodium LIDAR6320The Colorado State University (CSU) narrow-band sodium (Na) lidar is located at Fort Collins, Colorado at (40.59N, 105.14W), 1570 m above sea level. It was developed with CEDAR support and has been in operation since 1990. The sodium layer is located between about 70 and 120 km, with a peak near 92 km. At the end of 2001 at 92 km, the apex magnetic lat,lon coordinates were (49.61, -40.17), where the magnetic inclination and declination angles were 67.58 deg and 10.33 deg. The magnetic local time at 0 UT is 1612 MLT.These auroral and airglow data are on video tape at NCAR. The images are unprocessed raw data in black-and-white and then in false color. Corrections for average background and vignetting are possible using the false color images. If the user wants more in-depth analysis for a particular event or data set, or data beyond 1994, contact Michael Mendillo (mendillo@bu.edu). A web page is at http://www.bu.edu/csp/imaging_science. The presence of aurora is indicated by an '*' and the presence of aurora and SAR arcs by '**'. The Mobile Ionospheric ObservatoryMHIMillstone Hill Imagerhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:Millstone_Hill_Imager7240WFP5430Watson Lake, Canada Fabry-PerotThe Watson Lake Fabry-Perot interferometer, operated by the Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Sciences of the University of Michigan is located at latitude 60.055N and longitude 128.58W, and at an altitude of 2950 feet. The FPI operated from 11/91-4/92 and 11/92-5/93.
Currently, the interferometer observes the line profile of the forbidden emission OI (6300 A). The geophysical parameters obtained from the data reduction are the gas kinetic temperature of the emitting region from the natural width of the sky profile, the line of sight wind from the Doppler shift of the sky profile, and the surface brightness of the emission line. OI (6300 A) nightglow emission is generally believed to issue from the altitude range 175 to 500 km, with the major contribution originating from a narrow height interval (a few scale heights thick) centered roughly one neutral scale height below the altitude of maximum electron density. Thus, the peak altitude of emission and the parameters of the F region are interdependent and it is difficult to assign a unique altitude to each ground based OI (6300 A) interferometer measurement. If no other information is available, we generally ascribe 250 km as the altitude of emission.
Line of sight winds derived from the observed shift of the emission line from a zero reference position requires the determination of a zero wind. The reference zero wind is taken to be the average of an entire nights vertical wind data. Generally, the four cardinal directions are also sampled as well as the vertical. There is no exclusion of any data in the CEDAR Data Base, so cloudy night fits are also included. The cloud cover (code 440) measured by the Watson Lake meteorological station is given in octas of the sky covered. Values range from 0 (clear) to 9 (overcast).
Summary plots of the relative emission, neutral temeprature and vertical wind are plotted with error bars for the vertical look direction. For look directions in opposite cardinal directions, horizontal winds are plotted without error bars. For periods where there are plots of the vertical wind, but not of the horizontal wind, then the look directions are not cardinal. In the summary plots, wind measurements were not plotted unless the cloud cover was 0-3. Temperatures and relative emission measurements were not plotted unless the cloud cover was 0-6. For the period of data in the CEDAR Data Base, the cloud cover was 0-3 38% of the time, and 0-6 48% of the time.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:wfpMJFThe Fabry-Perot Interferometric Spectrometer at Mount John Observatory, New Zealand (43.98S, 170.42E) has been operated since 1991 by the Graduate Program in Geophysics, University of Washington, in cooperation with the Physics and Astronomy Department of the University of Canterbury, NZ, and the Geophysical Institute of the University of Alaska.Mount John New Zealand Fabry-Perothttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mjf50601340The Saskatoon MF radar is located in the province of Saskatchewan in Canada (52N, 107W). The solar local time (SLT) is Universal Time (UT) minus 7 hours and 10 minutes. (SLT = UT - 7:10). The phases are in SLT and the measurement days start at 0 UT. The Saskatoon MF radar has provided considerable mean winds (Manson et al., 1990a and 1991a) and tidal data (Manson et al, 1989) since 1979. LTCS-1 and LTCS-2 are described for all middle atmosphere radars in Manson et al (1990b,1991b). MF radars use the "spaced antenna" method. Harmonic analysis is applied to hourly mean winds (weighted by data yield per hour) at individual heights to obtain tides for the prime LTCS or stated intervals. Typical standard deviations for means, 12-hour and 24-hour tides are in the above LTCS papers. Tides of the month for Saskatoon are means of 4-day fits (the amplitudes are arithmetic means). Data up to 99 km are real heights --- above, they are from the E-region, a layer about 5 km centered near 102 km.
These are the analyzed data on the neutral winds in the mesosphere and lower thermosphere during or including the LTCS-1 period, 21-25 September 1987. This condensed format is consistent with the analyzed data from other sites as well, and is prepared in order to facilitate research work. However, users need to inform the data suppliers that they are using the data in case of updates or changes, and to insure that the data are being used and interpreted properly.Saskatoon Canada MF RadarSAFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:safThe CEDAR Database contains the 3-h Kp and ap indices, daily Ap, sunspot numbers and 10.7 cm solar flux values, and 81 day average 10.7 cm solar flux averages from 1 January 1960 to 30 April 2000. The 81 day average 10.7 cm solar flux is calculated, but our source for the other indices is the World Data Center in Boulder where one can get:
* Sunspot numbers (1818-present)
* 10.7 cm (2800 MHz) daily solar flux (1947-present), observed and adjusted to 1 A.U.
* Kp, ap and other indices (1932-present). These indices include Bartels solar rotation number, 3-h Kp, Kp sum, 3-h ap, daily Ap, Bartels solar rotation number, CP and C9 indices, international sunspot number, and 10.7 cm flux adjusted to 1 A.U. The Kp and ap indices are also defined. GPI210Geophysical indices from NGDC: Lenharthttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:gpihttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pla2200PLAPlatteville Colorado ST (MEDAC) RadarThe Platteville, CO ST (MEDAC) radar is located at (40 N, 105 W). The MEDAC (Meteor Echo Detection And Collection) sytem added to the ST (STratospheric) radar makes observations of winds measured from the backscatter off meteor trails. The system is described in Avery et al. (1990). The original observations are described in local time, which is 7 hours later than UT. (Mountain Standard Time = UT - 7 hours.) The mean solar local time (SLT) is about 7 hours after UT. (i.e., -105 E/15 deg/hr = -7.00 hours). Therefore, no adjustment was made to the phase, since the local time is very close to the solar local time.
These are the analyzed data on the neutral winds in the mesosphere and lower thermosphere during or including the LTCS-2 period, 5-10 December 1988. This condensed format is consistent with the analyzed data from other sites as well, and is prepared in order to facilitate research work. However, users need to inform the data suppliers that they are using the data in case of updates or changes, and to insure that the data are being used and interpreted properly.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:p4pP4P4470Poker Flat 4 Channel PhotometerThe Aerospace 4 channel filter photometer at Poker Flat, Alaska (65.12N, 212.57E) was developed to estimate the energy flux of auroral electrons, their average energy Eo (usually from 0.1 to 30 keV using a modified Gaussian or Maxwellian shape), and a scale factor fo for the atomic oxygen densities [O] from an MSIS model atmosphere. The [O] densities using the scaling factor fo can be compared to GUVI/TIMED estimates. The technique is only valid for clear night conditions where the solar zenith angle (sza) is greater than 102 deg (code 4102=1), and there is enough auroral emission (427.8 nm brightness, code 2421). Poker Flat apex magnetic coordinates are (65.44, -95.56) at 110 km in 2001, with 0 UT corresponding to 12.93 MLT. The magnetic inclination and declination angles are 77.41 deg and 24.89 deg. The photometer looks up the magnetic field line with a field of view (fov) of about 1 deg. The data rate can be programmed, but typically each channel is integrated for 1 sec, where the whole cycle including filter moves takes about 8 sec.
The 4 channels correspond to:
1. N2+ (427.8 nm, blue) first negative group (1NG) 0,1 molecular band
2. OI (630.0 nm, red) forbidden
3. OI (844.6 nm, eight) permitted
4. N2 (871.0 nm or 871.4 nm) first positive group (1PG) 2,1 molecular band The Digisonde (DGS-256) located at Qaanaaq, Greenland (77.5N, 290.6E) and operated by the University of Massachusettes Lowell Center for Atmospheric Research, for Phillips Laboratory Hanscom AFB, has produced ion velocity measurements and electron density profiles since 1983. The data are originally collected in local magnetic coordinates, and then converted to geographic coordinates using the declination angle of -71.0 for an altitude of 0 km.
The Digisonde generally operates in a 15 minute cycle mode, where the first 2-3 minutes an ionogram is recorded followed generally by 1-2 minutes of drift measurements, with the remaining 10-12 minutes idle. Sometimes the cycle time is 5 minutes. The range of altitudes is about 200-450 km, where the mean is about 300 km.
Digisondes transmit HF radio waves illuminating a large ionospheric area of several hundred kilomaters diameter over the sounder. Radio waves are sent up and reflected off orthogonal surfaces. Each reflection point is considered to be a separate source and has associated with it a line- of-sight (los) Doppler velocity measurement. Making the assumption that the main contribution to the measured Doppler shifts results from the uniform horizontal bulk motion of the plasma, the los velocity and source location are used to calculate the velocity vector by least squares fit.
The drift mode operated at Qaanaaq during 1989 resulted in up to a maximum of 64 sources in a single integration period of 5 seconds. One minute data is obtained where the error bar is the average of the standard deviations from 12 5-second integrations, while the value of each velocity component is the median from a further velocity distribution found using all the data points in the entire one minute period. The 1 minute results were taken and reported every 15 minutes. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:qadQADQaanaaq Greenland Digisonde29305980EUMhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eumA near infrared (NIR) BOMEM MB160 Michelson interferometer (MI) has operated at Eureka (80.22 N, 86.18 W), Canada, at 139 m above mean sea level since October, 1992.
The MI scans the dark sky NIR airglow emissions between ~5000-10000 cm-1. A periscope directs the airglow into the MI sequentially from four locations: overhead, and at an elevation angle of 25 deg at azimuth angles of 0 (geog N), 120, and 240 deg. The periscope dwells at each of the positions for about 8 min, averaging several scans. Airglow hydroxyl Meinel (OH-M) band emissions peak at 87 km and are located between about 83 and 89 km. For an elevation angle of 25 deg, the 87 km peak is located at a latitude spacing of 1.61 degrees, or about 179 km away. Eureka, Canada Michelson InterferometerThe Halley HF radar is located in Antarctica (76 degs S, 26 deg W) and overlooks a section of ionosphere poleward of 78 deg that covers much of eastern Antarctica and includes South Pole station. The field -of-view is conjugate to the west coast of Greenland and the Goose Bay HF radar. It has operated since 1988. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Halley velocity data is located at Syowa, Antarctica.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15) ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz) iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70) iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is approximately 50 deg wide and is centered on 165 deg E of N. HHF820http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:hhfHalley Antarctica HF RadarChatanika AK I.S. Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:cht50The incoherent scatter transmitter station at Chatanika, Alaska (65.1N, 147.4W) operated between 1971 and 1982. It was moved to Sondrestrom in 1982-1983, where it has been in operation since 1983. There are generally 7 record types (KINDAT) for each Chatanika experiment that are usually inputs or outputs to a program called VAST, which calculates electric fields, vector velocities and conductivities. VAST assumes the velocity field varies linearly with time. Data from five positions are used to find the three line-of-sight velocities at the time of the middle observation. Full error propagation, including covariance terms, is included. The density and temperature data are combined to obtain a spatial average for the time of the middle observation.
In addition, several criterea involving the least squares fit, as well as relative absolute uncertainties, have been examined to determine whether the derived F-region vector velocities are converted to electric fields, and the good values are height integrated to find the best possible estimate of the electric field. Starting in the D-region, the averaged electron densities are used to calculate the conductivities. The calculation has been improved to explicitly include the ion-neutral collision frequencies and to include a model atmosphere. CHTSondrestrom Fjord Michelson Interfer.5900http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sfmA near infrared (NIR) BOMEM MB160 Michelson interferometer (MI) has operated at Sondrestrom Fjord (66.99 N, 50.95 W), Greenland, 180 m above mean sea level since September, 1990.
The MI scans the dark sky NIR airglow emissions between ~5000-10000 cm-1. A periscope directs the airglow into the MI sequentially from three locations at an elevation angle of 25 deg at azimuth angles of 0 (geog N), 120, and 240 deg. The periscope dwells at each position for about 15 min. Airglow hydroxyl Meinel (OH-M) band emissions peak at 87 km and are located between about 83 and 89 km. For an elevation angle of 25 deg, the 87 km peak is at a latitude spacing of 1.61 degrees, or about 179 km away. SFMThe fixed-gap imaging Fabry-Perot Spectrometer (FPS) or Interferometer (FPI) at Inuvik in the North West Territories (NWT) of Canada (68.33N, 133.50W) is located on a hill above the Mackenzie River close to the Arctic Ocean. It is 103.2 m above mean sea level and has been operating since late 1998, with reliable data after about February 2000. It is operated by the Geophysical Institute of the University of Alaska, in cooperation with Environment Canada. Chris Strube, and previously Jeff Allen, helps to keep things running.IKF5510Inuvik NWT Fabry-Perot Interferometerhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ikfhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mlhThe incoherent scatter transmitter station at Millstone Hill, Massachusetts (42.6N, 71.5W) has been in operation since 1960. The facility is part of and operated by the Massachusetts Institute of Technology.
ISR data comes from the fixed zenith antenna, the steerable antenna, or both.
The electron densities from the power profile were calibrated with an on-site ionosonde, where recently, this ionosonde has been the University of Massachusetts at Lowell digisonde. Since the Coast Guard uses some of the frequencies needed to properly scan the ionosphere, calibration can sometimes be difficult. The calibrated electron density is then corrected for Te and Ti effects, where Te and Ti come from auto-correlation fits. The calibration and auto-correlation fits now have the same height resolution, although in the past, the auto-correlation fits had lower height resolution.
The ion composition changes from mostly O2+ and NO+ at lower altitudes, to mostly O+, and then to H+ and some He+ at higher altitudes. Above 400 km, the percent H+ is computed along with the major ion O+. At lower altitudes, the ratio of molecular ions to the total number of ions is modeled as specified by the FORTRAN code segment below.
REAL FUNCTION PMF(Z)
Z1=AMIN1(-(Z-120.)/40.,50.)
H=10.-6.*EXP(Z1)
Z2=AMIN1(-(Z-180.)/H, 50.)MLH3232Millstone Hill: zenith UHF antenna5140http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aqfArequipa, Peru Fabry-PerotAQFThe Fabry-Perot interferometer of the Arequipa Automatic Airglow Observatory (A3O) is operated jointly by the University of Pittsburgh and Clemson University under grants from the NSF Atmospheric Sciences Aeronomy division, with space and on-site technical support provided by the NASA Laser Satellite Tracking Station near Arequipa, Peru. The station is located at latitude 16.47 S and longitude 71.49 W at an elevation of 2489 m. The apex magnetic latitude is about -12, with a magnetic dip latitude of about 3, an inclination angle of -6 to -7, and a declination between +1 and -2 between 1983 and 1999. The mean local solar time is behind UT by 4 hours and 46 minutes (-71.49/15 = -4.766 = -4h 46m). The FPI uses the atomic oxygen filter at 630.0 nm, where the approximate emission height is assumed to be about 250 km.Platteville, Colorado MF RADARhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltrThe Platteville 2 MHz MF radar is located in Colorado, USA (40.18N, 104.7W; 1505 m alt), and has been in operation since December 1999, with a data gap from March to July 2000 because of system problems. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (49.3, -39.6) degrees. The magnetic inclination and declination angles were 67.2 deg and 10.0 deg. The magnetic local time at 0000 Universal Time (UT) is about 1617 MLT. The solar local time (SLT) is UT minus 6 hours and 59 minutes (-104.7/15=-6.98).1285PLRThe Goose Bay HF radar is located in central Labrador (53.3 deg N, 299.56 deg E) and overlooks a section of ionosphere poleward of 55 deg N that covers northeastern Canada (Labrador, Baffin Island), the Davis Strait and Baffin Bay, and southern and central Greenland. It has operated since 1983. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Goose Bay velocity data is located at Stokkseyri in western Iceland.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second array was added in 1985 to provide the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-50), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. Typical beam integration times are 5 and 6 sec, corresponding to scan repeat times of 80 and 96 sec, respectively. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is eastward approximately 50 deg wide and is centered on 5 deg E of N. 870GBFGoose Bay HF Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:gbfThe Global Scale Wave Model (GSWM) simulates solar diurnal and semidiurnal tides calculated in the Earth's atmosphere using realistic ozone and water vapor forcing. The calculations were done for 4 months (January, April, July, October), where the day assumed was the 15th of each month. The background winds are calculated assuming geostrophic balance between 20-80 km. Above 80 km, they are taken from the Portnyagin and Solov'eva model, and below 20 they are taken from the Groves/MSIS model. The background temperature and density are taken from the MSISE90 model using a solar flux of 120 and an Ap of 4.
The results are only weakly dependent on solar cycle, so the year is arbitrary. The year 1995 was chosen because this was the year that the reference appeared. The diurnal and semidiurnal amplitudes and phases of the neutral temperature, the eastward neutral wind, the northward neutral wind, and the vertical neutral wind are given for 31 altitudes between 0 and 124 km in steps of approximately 4 km. There are 59 geographic latitudes that vary between 87 and -87 in steps of 3 degrees. The tidal results are zonal averages. The results from this set of calculations are now known as GSWM-95 tidal predictions.
The vertical velocity is defined to be 0 at the surface, but other temperature and wind values may be zero with a non-zero phase due to round-off. http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:gswGSWM solar diurnal & semidiurnal tides322GSWSacramento Peak NM SpectrometerSacramento Peak NM SpectrometerSAChttp://nsosp.nso.edu/4733SDT320These are the results of model runs at 170 altitudes between 0 and 110 km at every 2 degrees of latitude between -88 and +88. We give the semidiurnal amplitude and phase of the eastward neutral wind, the northward neutral wind, the neutral temperature, and the geopotential. The results are independent of solar cycle, so the year is arbitrary. The year 1988 was chosen because this was the year that the model runs were made. The calculations were done for each month of the year (on the 15th day of the month). Some temperature amplitudes are shown as 0 near the pole but with some phase. This is the result of truncation with amplitudes less than 0.005 K.Forbes/Vial Model Semidiurnal Tideshttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:sdtSouth Pole Fabry-Perot Interfer SpectrThe Fabry-Perot Interferometric Spectrometer at Amundsen-Scott South Pole Station (90.00S) has been operated since 1989 by the Department of Earth and Space Sciences, University of Washington, in cooperation with the Geophysical Institute of the University of Alaska. The instrument is located within 150 feet of the South Pole at 2835 m above mean sea level. The geographic longitude is used to reckon the azimuthal direction of observation, with 0 E corresponding to 0 deg azimuth. The apex magnetic coordinates of South Pole at 250 km height in 1992 were (-74.4, 17.7), with a magnetic declination of -21.37 deg (or 158.63 E toward the compass south pole), an inclination of -74.78 deg, and 0 UT at 2039 MLT. The invariant (apex) South Pole at 250 km height was at (74.2S, 126.0E), and the perpendicular to the magnetic latitude circle pointed to 125.6E. Hernandez et al (1991) used magnetic south towards 120 E, with 0 UT at 2023 MLT. The magnetic grid is useful for ordering the red line observations at about 250 km height, but not for other observations from emissions below 100 km height.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:spfSPF5000DBMhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dbmA near infrared (NIR) BOMEM DA-8 Michelson interferometer (MI) has operated at Daytona Beach (29.19 N, 81.05 W), Florida, USA, 0 m above mean sea level since September, 1996.
The MI scans the dark sky NIR airglow emissions between ~5000-10000 cm-1. A periscope directs the airglow into the MI sequentially from three locations at an elevation angle of 25 deg at azimuth angles of 0 (geog N), 120, and 240 deg. The periscope dwells at each position for about 5 min. Airglow hydroxyl Meinel (OH-M) band emissions peak at 87 km and are located between about 83 and 89 km. For an elevation angle of 25 deg, the 87 km peak is at a latitude spacing of 1.61 degrees, or about 179 km away. Daytona Beach FL, USA Michelson Inter.57207191http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mtmMTMUSU Mesospheric Temp Mapper CCD ImagerThe Utah State University (USU) CEDAR Mesospheric Temperature Mapper (MTM) is a mobile CCD imager that has been operated in several mid and low latitude locations since its construction was completed in 1996. The imager was built to investigate mesospheric temperature and wave induced variability using the [OH] emission (mean altitude 87 km). In March of 1996 it was tested at Bear Lake Observatory (BLO) (41.933N, 111.417W, 1981 m) and took data at BLO between 7-18 Oct 1996, 4-15 May 1997, and 4 Aug - 24 Sep, 1998. For a year between 11 June 1997 and 2 June 1998, the MTM took data alongside the Colorado State University Na Temperature lidar at Fort Collins, Colorado (40.590N, 105.140W, 1570 m). It was moved to the Starfire Optical Range (SOR) near Albuquerque, New Mexico (34.9639N, 106.4619W), and took data from October 1998 to Dec 1999 alongside the University of Illinois Wind Temperature lidar and all-sky imager and University of Western Ontario Meteor radar. The MTM was then upgraded at USU to include a capability to measure mesospheric temperature using the [O2] nightglow emission (mean altitude 94 km) as well as the [OH] emission. It was then tested and operated at BLO during the period Oct 2000-June 2001. Most recently it was deployed to Maui, Hawaii (20.75N, 156.24W) to take data from October 2001 until the present. The latter data (KINDAT=17087 for OH and KINDAT=17094 for O2) are currently available as nightly mean determinations of [OH] and [O2] rotational temperatures centered at 87 and 94 km, respectively. These data also provide relative band intensities. Higher temporal resolution data are available on request to USU. They start in 2002 to coincide with the TIMED satellite instrumentation deployment.
The USU MTM is a CCD imager that measures the hydroxyl [OH] Meinel nightglow in the (6,2) rotational band and the o2 (0,1) molecular oxygen band, both emissions occurring in the near infrared (NIR). The [OH] rotational temperature is derived from the intensity ratio of the P1(4)/P1(2) lines within the (6,2) rotational band. The rotational temperature should be close to the atmospheric temperature under normal equilibrium conditions. The [OH] emission layer is centered near 87 km (+/-2 km) with a thickness of about 8 km. The O2 emission originates at somewhat higher mean altitude of 94 km but has a similar effective layer thickness (FWHM) of about 8 km. Together these measurements permit the investigation of mesospheric temperature variability at two closely spaced but separate regions important for wave-induced (gravity wave, tides and planetary wave) as well as seasonal and longer term variations. Data in the CEDAR Database from the University of Illinois lidar are in three separate areas:
- Arecibo AIDA-89 campaign, U of IL Na Lidar
- Hawaii ALOHA-90 campaign, U of IL Na Lidar
- Urbana Fe measurements, U of IL Fe Lidar
- Urbana Tn/Wn/Na measurements, U of IL Na Lidar, 1996-1998http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:uilufehttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:uilunaUILhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:uilanahttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:uilhnahttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:uilU of Illinois LIDAR6300SSDhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:ssd2890The Digisonde (DISS) located at Sondre Stromfjord, Greenland (67.0N,309.05E) and operated by the University of Massachusettes Lowell Center for Atmospheric Research, for Air Force Research Laboratory Hanscom AFB, has produced ion velocity measurements and electron density profiles since 1986. The data are originally collected in local magnetic coordinates, and then converted to geographic coordinates using the declination angle of -41.2 for an altitude of 0 km.
The Digisonde generally operates in a 15 minute cycle mode, where the first 2-3 minutes an ionogram is recorded followed generally by 1-2 minutes of drift measurements, with the remaining 10-12 minutes idle. Sometimes the cycle time is 5 minutes. The range of altitudes is about 200-450 km, where the mean for the 1993 data was set to 250 km.
Digisondes transmit HF radio waves illuminating a large ionospheric area of several hundred kilomaters diameter over the sounder. Radio waves are sent up and reflected off orthogonal surfaces. Each reflection point is considered to be a separate source and has associated with it a line- of-sight (los) Doppler velocity measurement. Making the assumption that the main contribution to the measured Doppler shifts results from the uniform horizontal bulk motion of the plasma, the los velocity and source location are used to calculate the velocity vector by least squares fit.
The drift mode resulted in up to a maximum of 64 sources in a single integration period of 5 seconds. One minute data is obtained where the error bar is the average of the standard deviations from 12 5-second integrations, while the value of each velocity component is the median from a further velocity distribution found using all the data points in the entire one minute period. The 1 minute results were taken and reported every 15 minutes. Sondre Stromfjord Digisondehttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aopAOPAbastumani Photometers4335The Abastumani Astrophysical Observatory is located in Tbilisi, Georgia (41.8? N, 42.8? E; ~1700m msl alt). There are several instruments that collect nighttime optical observations, spectrographs and photometers, with the earliest observations made in 1942. The spectrograph data is on film and the older photometrical data for the red/green [O] lines are on paper charts. However, the length of the data set makes it attractive for long-term studies if the data could be digitized. Nighttime brightness observations come from:
1. Spectrograph (light scattering) is all on film
1. 1942-1957
2. 1957-1992 (new instrument?)
3. 1992-1999 gap
4. 1999-present
2. Photometer with filters for [O] green (557.7nm) and red (630.0nm)
1. 1957-1974 resolution about 30 min on paper charts
2. 1974-1993 resolution 3 min for each filter used (3 filters with the OH band filter (8-3) R1(??) branch centered on 726.4 nm(???))
OH(8-3) R1 from Chamberlain, p 370, Physics of the Aurora and Airglow
K''=1 724.48
K''=2 723.98
K''=3 723.80
K''=4 723.92
K''=5 724.42
K''=6 725.33
K''=7 726.51 1993-2000 gap 2000-present same 3 min resolution
3. Na doublet (????nm) from 1957 to present (gaps? changes in instruments or filters?)
4. Photometer OH bands (filters for 6-1, 9-3, etc??) from 1957-1974, intermittent thereafter. Sometimes used 1 filter, 2 filters, or 3 filters (??).
1. 1958-1970 (missing 1965-1967) OH(9-3) and OH(6-1) P1 branches (J=3/2) centered at 635 nm and 660 nm (? kindats 6350 and 6600): Have arbitrary brightness for entire night (Fishkova et al REF???) Second nm numbers are from Chamberlain, p 370, Physics of the Aurora and Airglow
OH(9-3) OH(6-1)
P1 628.7 628.76 653.3 653.31
P2 630.6 630.68 655.4 655.37
P3 632.9 632.92 657.4 657.73
P4 635.6 635.51 660.3 660.41
P5 638.6 638.44 663.3 663.42
P6 642.0 641.69 666.7 666.75
2. 1987-1993 OH(6-1) R1 branch centered at 647.3 nm (kindat=6470) between 64?.? nm and 64?.? nm (or wavenumber) every 3 min pointed at azimuth 180 (geographic south) and 42 deg elevation angle above the horizon with a field-of-view of ???.
OH(6-1) R1 from Chamberlain, p 370, Physics of the Aurora and Airglow
K''=1 647.10
K''=2 646.60
K''=3 646.36
K''=4 646.38
K''=5 646.69
K''=6 647.28
K''=7 648.17
5. Geocorona H alpha resonance line (???? nm)
1. 1958-1993
2. 1993-? gap
6. O3 total content from 1965-1993
Many of the early observations from 1957-1993 were made by Prof. L. Fishkova and Dr. N. Marcvaladze. After the mid 1970's, they used the Einstein Transition Probabilities from Mies (1974).Coupling, Energetics and Dynamics of Atmospheric Regions data archiveDSThttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:dstThe CEDAR Database contains hourly Dst values calculated from lower latitude ground magnetometers between 1 January 1957 and 31 March 2000. Other sources for Dst (1957-present) are:
* Dst (1957-present) from the World Data Center in Japan
* Dst (1957-present) from the World Data Center in Boulder Geophysical indices from NGDC: Dst2125340Millstone Hillhttp://www.haystack.mit.edu/homepage.htmlThe Millstone Hill Observatory, located in Westford, Massachusetts, is a broad-based atmospheric sciences research facility owned and operated by the Massachusetts Institute of Technology.The Millstone Hill Fabry Perot interferometer is operated by MIT in cooperation with the University of Pittsburgh. The interferometer is located near the Millstone Hill incoherent scatter radar at latitude 42 degrees 37 minutes North (42.62) and longitude 71 degrees 27 minutes West (-71.45). Mean local solar time differs from UT by -(4 hour 46 minutes). The local magnetic field has a 15 degree variation to the West and an inclination of 72 degrees.MFP42.62Millstone Hill Fabry-Perot-71.45http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mfphttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:stsSTS40The incoherent scatter transmitter station at St. Santin, France (44.6N, 2.2E) operated between 1963 and 1987. The CEDAR Data Base holds all the data taken from 1966 until the end. Up until June 1973 and after July of 1986, the only receiver station operating was located at Nancay (47.4N, 2.2E). Between 1973 and 1986, 2 other receivers also operated at Montpazier (44.7N, 0.8E) and at Mende (44.5N, 3.45E).
In general, the daytime height range is 105 to 350 km, while the nighttime height range is 200 to 500 km. Before January 1, 1969, the faraday correction is not taken into account in the computation. The spectrum are analysed following the scheme described in Waldteufel (1970). The ion drift component is quasi parallel to the magnetic field as measured by the Nancay receiving station. Because the transmitter is not located at the receiving location, the bisector velocity is plotted for the period when only Nancay data were received. When all 3 receivers were on, then the data are 30 minute averages and the ion drifts in the geomagnetic coordinate system are calculated.Saint Santin I.S. Radar40PFX170The CEDAR Database contains 16-s instegrations of the ion and electron "characteristic energy" and energy flux from NOAA SEM-2 satellites (NOAA-15, NOAA-16, NOAA-17) from June 1998 to December 2004http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:pfxSpacecraft Particle FluxPoker Flat Alaska MF Radar1375RPKhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:rpkThe Poker Flat, Alaska (65.126 N, 147.495 W; alt 208 m) 2.43 MHz MF radar has been in operation since 1998. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (65.4, -95.5) degrees. The magnetic inclination and declination angles were 77.4 deg and 24.1 deg. The magnetic local time at 0 Universal Time (UT) is about 1233 MLT. The solar local time (SLT) is UT minus 9 hours and 50 minutes (-147.495/15.=-9.833).
The original data files are 30 min averages of the zonal, meridional and 'vertical' velocity in UT. The UT time is the midpoint UT, and is also listed as the midpoint SLT. Samples are taken every 3, 4 or 5 min, so 6 to 10 samples can be had between UT 23:45:00 and UT 00:15:00. To improve data quality, 'median screening' is applied inside a 1-h bin. If data points lie outside a threshold standard deviation (code 4152) of usually 1.5 inside a 1-hr bin, they are discarded. So the low qulity (jamped) data are rejected and then the remaining data are averaged over 30-min bins with a threshold of usually 30% (code 4151). The number of points used in each direction are in codes 422, 423 and 424.
The 'vertical' velocities (code 1432, 'contaminated neutral vertical geographic wind (+up)') are from the beam in the vertical direction. The antenna array in a triangle has a different beam width for different azimuth direction, resulting in beam widths about 20-30 deg wide. Hence, the 'vertical' velocity will be contaminated by horizontal wind times the sine of 10 to 15 degrees (.17 to .26). Since the horizontal winds are stronger than the vertical winds, even the sign could be incorrect. The standard deviations of the 'vertical' winds are also larger than the average values.
The MF operating frequency is 1.95550 MHz, with a peak transmitter power of 50 kW. The radar operates as a spaced-antenna system (Vincent, 1986), relying on coherent echo signals from middle atmosphere ionization. The inter-pulse period is 12.5 millisec during the day and 25 millisec during the night. There are 80 coherent integrations during the day and 40 at night, using 240 samples in the full correlation analysis (FCA) of Briggs [1984] with built-in rejection criteria. [ie, if want 240 sec or 4 min integration during day and night, then 12.5x10-3sec * 80 integ * 240 samples = 240 sec and 25x10-3sec * 40 integ * 240 samples = 240 sec.]
Data sampling is done every 2 km usually between 60-98 km for Yamagawa (60-108 km for Wakkanai, 44-108 km for Poker Flat). The height range of wind velocity data is variable accoding to atmospheric and radio conditions and is usually about 70-90 km at Yamagawa and Wakkanai during the day and 80-90 km at night (60-90 km/70-90 km for Poker Flat for day/night conditions).
The pulse width is 48 microsec (27 microsec before September 1996), giving a height resolution of approx. 7.2 km (4.1 km) assuming a simple rectangular wave pulse. For the 48-microsec case, the range of heights illuminated by the wave pulse = velocity of light * pulse-width / 2 = 3x10**8 m/s * 48x10-6s / 2 = 7.2 km. However, neutral velocities are given every 2 km. 45KKVThe Kharkov incoherent scatter radar is located at (49.7N, 36.3E; 97 m above mean sea level) in Ukraine. Operations started around 1981. There are 2 antennas, a zenith antenna and a steerable antenna, but both are assigned the same kinst of 45, and the elevation angle will determine which is being used.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:kkvKharkov Ukraine I.S. RadarThe dispersing element of the spectrometer is an air-spaced, 14 cm diameter effective clear-aperture Fabry-Perot interferometer, which is self-aligning and self-stabilizing (Hernandez and Mills, 1973). The instrument was operated at the optimum point for kinetic temperature determinations (Hernandez, 1979; 1988).
The spectrometer operated with narrow (<0.3 nm wide) interference filters -a necessity, in particular, for the 630.0 nm emission, in order to avoid contamination from the nearby OH emission lines (Hernandez, 1974). The inherent stability of the spectrometer is about 0.5 m/s (632.8 nm) for periods of months, because of its self-stabilizing properties. The instrumental internal stability calibration is updated every 9 s throughout the day, year round.
The spectrometer observed wavelength with the Fritz Peak (FPO or fpf) and Ann Arbor (AAM or aaf) instrument has been the so-called red line (630.0 nm, kindat=17001, 1973-1985 at FPO and 1986-1987 at AAM) of atomic oxygen (OI) with typical emission height peak in the range 210 to 300 km.
The spectrometer observed the night-sky at the 4 cardinal directions at 20-degree elevation above the horizon, as well as zenith. Since the instrument is light-limited, the time spent in observing this 5-direction cycle can be as short as 5 minutes during auroral activity. The instrument is internally time-limited to spend no less that one-minute and no more than 15 minutes in any given direction. Other observing protocols, such as two orthogonal directions and zenith, have also been used. The observations were made every evening and only those with clear weather -as reported by an observer on site- are reported here. Because of the narrow filters used, operation of the instrument is not affected by moonlight. Typically, about 30% of the nights observed were clear.http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:aaf5292Ann Arbor MI Fabry-Perot Interf SpAAFhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:fhfFHFHankasalmi Finland HF Radar900The Hankasalmi HF radar is located in southern Finland (62.32 deg N, 26.61 deg E) and looks to the west over a section of ionosphere that includes the Greenland sea and Svaalbard. It has operated since 1995. The facility is part of the SuperDARN network of HF radars that extends from western North America to Scandinavia in the Northern hemisphere and covers much of Antarctica in the Southern hemisphere. The SuperDARN radar for the most direct 2-D merging of Hankasalmi velocity data is located at Pykkvibaer, Iceland.
The radar forms and steers its beam by the phasing of transmissions from 16 elements in a linear antenna array. A second 4-element array provides the capability to measure elevation angle. The basic radar operation consists of the following steps: i) selection of a beam position (0-15), ii) search for the quietest 5-kHz channel about the assigned transmitting frequency (8-20 MHz), iii) repeated transmission of a multi-pulse sequence over the selected integration period and reception of backscattered signal with gating in range (1-70), and iv) calculation of the auto-correlation functions (ACFs). These operations are usually carried out in sequence for the 16 beam positions, which collectively constitute 1 scan. The beam integration period is typically 6 or 7 sec, and the scan repeat time is 96 sec or 120 sec. Within a scan, beam 0 corresponds to the most westward beam position and beam 15 to the most eastward. The azimuth sector scanned is westward approximately 50 deg wide and is centered on -12 deg E of N. 1560ATMhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:atmBetween August 1974 and April 1987, the Georgia Tech Radio Meteor Wind Facility was in routine operation, measuring winds between 80 and 100 km over Atlanta, Georgia, USA. A series of technical reports has been published on the measurements (Roper, 1978; 1982; 1984; 1987).
At meteor heights, the viewing area was a slab 400 km in diameter across. Significant results were achieved by averaging from 5 days to 2 weeks of data. The local mean solar time for Atlanta is the Universal Time minus 5 hours and 37 minutes. The tabulations are the result of matching the data against the model developed by Groves (1959). The model assumes cubic variations with height H for prevailing, diurnal and semidiurnal components of the horizontal wind. Atlanta Georgia Meteor Wind Radarhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltr1221RTHThe Rothera, Antarctica (67.57S, 68.12W; ~5 m alt) 1.98 MHz MF radar was in operation 1997-1998, and was reinstalled in 2002. The data are noisy. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (-52.6, 7.6) degrees. The magnetic inclination and declination angles were -59.9 deg and 20.5. deg. The magnetic local time at 0000 Universal Time (UT) is about 1925 MLT. The solar local time (SLT) is UT minus 4 hours and 32 minutes (-68.12/15.=-4.5413).Rothera, Antarctica MF RADAR95ESRhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:esrThe EISCAT (European Incoherent SCATter) Svalbard Radar (ESR) consists of a transmitter and receiver in Longyearbyen, Norway (78.15N, 16.04E; 75.0 magnetic N). Observations were begun in 1996. The system was added to the EISCAT KST (Kiruna/Sodankyla/Tromso) tri-static facility in Scandinavia, which has its own web page.
There are several common programs used for the World Days, which are a part of the CEDAR Database from the KST site, but not yet on a regular basis from the ESR site. There are many other experimental times which should be accessed with the aid of an EISCAT colleague.
The power profiles are calibrated with an on-site ionosonde, and are then corrected for Te and Ti effects which are deduced from the auto-correlation functions (ACFs). The collision frequency model used is the CIRA 1972 model atmosphere in Banks and Kockarts (1973), in Aeronmy Part A. The NO+ composition is assumed zero above 300 km. Svalbard I.S. RadarEIS74http://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:eisThe EISCAT (European Incoherent SCATter) facility in Scandinavia consists of a transimitter/receiver station at Tromso, Norway (69.6N, 19.2E), and receiver stations at Kiruna, Sweden (67.9N, 20.4E) and Sodankyla, Finland (67.4N, 26.6E). The facility has been in operation since 1981, and recently expanded to include a facility at Svalbard, which will have its own web page when data are included in the CEDAR Data Base.
74EISCAT: Tromso VHF RadarEsrange, Sweden Meteor RADARhttp://cedarweb.hao.ucar.edu/wiki/index.php/Instruments:mltrThe Esrange, Sweden (67.89N, 21.08E; alt ??? m) 32.5 MHz meteor radar has been in operation since August 1999. On day 359 of 2001 at 89 km altitude, the apex magnetic coordinates were (64.8, 103.2) degrees. The magnetic inclination and declination angles were 77.2 deg and 5.8 deg. The magnetic local time at 0 Universal Time (UT) is about 0148 MLT. The solar local time (SLT) is UT plus 1 hour and 24 minutes (21.08/15=1.405).1775EMR